---
OA_place: repository
OA_type: green
_id: '21230'
abstract:
- lang: eng
  text: Asteroseismology is the study of the interior physics and structure of stars
    using their pulsations. It is applicable to stars across the Hertzsprung–Russell
    (HR) diagram and a powerful technique not only to measure masses, radii, and ages
    but also directly constrain interior rotation, chemical mixing, and magnetism.
    This is because a star's self-excited pulsation modes are sensitive to its structure.
    Asteroseismology generally requires long-duration and high-precision time-series
    data. The method of forward asteroseismic modeling, which is the statistical comparison
    of observed pulsation mode frequencies to theoretically predicted pulsation frequencies
    calculated from a grid of models, provides precise constraints for calibrating
    various transport phenomena. In this introduction to asteroseismology, we provide
    an overview of its principles, and the typical data sets and methodologies used
    to constrain stellar interiors. Finally, we present key highlights of asteroseismic
    results from across the HR diagram, and conclude with ongoing challenges and future
    prospects for this ever-expanding field within stellar astrophysics.
article_processing_charge: No
arxiv: 1
author:
- first_name: Dominic M.
  full_name: Bowman, Dominic M.
  last_name: Bowman
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
citation:
  ama: 'Bowman DM, Bugnet LA. Asteroseismology. In: Mandel I, ed. <i>Encyclopedia
    of Astrophysics</i>. Vol 2. Elsevier; 2026:133-153. doi:<a href="https://doi.org/10.1016/b978-0-443-21439-4.00036-5">10.1016/b978-0-443-21439-4.00036-5</a>'
  apa: Bowman, D. M., &#38; Bugnet, L. A. (2026). Asteroseismology. In I. Mandel (Ed.),
    <i>Encyclopedia of Astrophysics</i> (Vol. 2, pp. 133–153). Elsevier. <a href="https://doi.org/10.1016/b978-0-443-21439-4.00036-5">https://doi.org/10.1016/b978-0-443-21439-4.00036-5</a>
  chicago: Bowman, Dominic M., and Lisa Annabelle Bugnet. “Asteroseismology.” In <i>Encyclopedia
    of Astrophysics</i>, edited by Ilya Mandel, 2:133–53. Elsevier, 2026. <a href="https://doi.org/10.1016/b978-0-443-21439-4.00036-5">https://doi.org/10.1016/b978-0-443-21439-4.00036-5</a>.
  ieee: D. M. Bowman and L. A. Bugnet, “Asteroseismology,” in <i>Encyclopedia of Astrophysics</i>,
    vol. 2, I. Mandel, Ed. Elsevier, 2026, pp. 133–153.
  ista: 'Bowman DM, Bugnet LA. 2026.Asteroseismology. In: Encyclopedia of Astrophysics.
    vol. 2, 133–153.'
  mla: Bowman, Dominic M., and Lisa Annabelle Bugnet. “Asteroseismology.” <i>Encyclopedia
    of Astrophysics</i>, edited by Ilya Mandel, vol. 2, Elsevier, 2026, pp. 133–53,
    doi:<a href="https://doi.org/10.1016/b978-0-443-21439-4.00036-5">10.1016/b978-0-443-21439-4.00036-5</a>.
  short: D.M. Bowman, L.A. Bugnet, in:, I. Mandel (Ed.), Encyclopedia of Astrophysics,
    Elsevier, 2026, pp. 133–153.
date_created: 2026-02-16T10:43:01Z
date_published: 2026-01-01T00:00:00Z
date_updated: 2026-02-17T11:05:20Z
day: '01'
department:
- _id: LiBu
doi: 10.1016/b978-0-443-21439-4.00036-5
editor:
- first_name: Ilya
  full_name: Mandel, Ilya
  last_name: Mandel
external_id:
  arxiv:
  - '2410.01715'
intvolume: '         2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.2410.01715
month: '01'
oa: 1
oa_version: Preprint
page: 133-153
publication: Encyclopedia of Astrophysics
publication_identifier:
  isbn:
  - '9780443214400'
publication_status: published
publisher: Elsevier
quality_controlled: '1'
scopus_import: '1'
status: public
title: Asteroseismology
type: book_chapter
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 2
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21658'
abstract:
- lang: eng
  text: Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential
    rotation between the core and the envelope of evolved solar-like stars. Quadrupolar
    (ℓ = 2) mixed modes also contain information regarding internal dynamics but are
    very rarely characterised due to their low amplitude and the challenging identification
    of adjacent or overlapping rotationally split multiplets affected by near-degeneracy
    effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond
    ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed
    modes while explicitly accounting for near-degeneracy effects that distort their
    rotational multiplets. We have derived a new asymptotic formulation of near-degenerate
    mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction
    between modes of adjacent radial orders. This formalism, expressed directly in
    the mixed-mode basis, provides analytical expressions for the near-degeneracy
    effects. We implemented the formalism within a global Bayesian mode-fitting framework
    for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were
    able to asymptotically model the asymmetric rotational splitting present in various
    radial orders of ℓ = 2 modes observed in young red giant stars without the need
    for any numerical stellar modelling. We applied our formalism to the Kepler target
    KIC 7341231, and it yielded core and envelope rotation rates consistent with previous
    numerical modelling while providing improved constraints from the global and model-independent
    approach. We also characterised the new target, KIC 8179973, measuring its rotation
    rate and mixed-mode parameters for the first time. As our framework relies on
    a direct global fit, it allows for much better precision on the asteroseismic
    parameters and rotation rate estimates than standard methods, yielding better
    constraints for rotation inversions. We have placed the first observational constraints
    on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving
    the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.
acknowledgement: 'We thank the referee for their careful and constructive report,
  which has substantially enhanced both the quality and clarity of the manuscript.
  L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research
  Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement
  N°101165631). While partially funded by the European Union, views and opinions expressed
  are, however, those of the authors only and do not necessarily reflect those of
  the European Union or the European Research Council. Neither the European Union
  nor the granting authority can be held responsible for them. The authors acknowledge
  the great support and feedback provided during the redaction of this article by
  Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt
  for her insights on uncertainty estimates. The authors also thank the members of
  the Asteroseismology and Stellar Dynamics group of the Institute of Science and
  Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K.
  Smith. This paper includes data collected by the Kepler mission and obtained from
  the MAST data archive at the Space Telescope Science Institute (STScI). Funding
  for the Kepler mission is provided by the NASA Science Mission Directorate. STScI
  is operated by the Association of Universities for Research in Astronomy, Inc.,
  under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013,
  2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et
  al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017),
  slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011),
  sloscillations (Kuszlewicz et al. 2019, 2023).'
article_number: A321
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Bastien Raymond Bernard
  full_name: Liagre, Bastien Raymond Bernard
  id: 662f1873-cab4-11f0-a719-8087d302868d
  last_name: Liagre
- first_name: Aayush A
  full_name: Desai, Aayush A
  id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e
  last_name: Desai
- first_name: Lukas
  full_name: Einramhof, Lukas
  id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c
  last_name: Einramhof
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
citation:
  ama: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar
    mixed modes: From an asymptotic description to data fitting. <i>Astronomy and
    Astrophysics</i>. 2026;707. doi:<a href="https://doi.org/10.1051/0004-6361/202558023">10.1051/0004-6361/202558023</a>'
  apa: 'Liagre, B. R. B., Desai, A. A., Einramhof, L., &#38; Bugnet, L. A. (2026).
    Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
    to data fitting. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202558023">https://doi.org/10.1051/0004-6361/202558023</a>'
  chicago: 'Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and
    Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From
    an Asymptotic Description to Data Fitting.” <i>Astronomy and Astrophysics</i>.
    EDP Sciences, 2026. <a href="https://doi.org/10.1051/0004-6361/202558023">https://doi.org/10.1051/0004-6361/202558023</a>.'
  ieee: 'B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy
    effects in quadrupolar mixed modes: From an asymptotic description to data fitting,”
    <i>Astronomy and Astrophysics</i>, vol. 707. EDP Sciences, 2026.'
  ista: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects
    in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy
    and Astrophysics. 707, A321.'
  mla: 'Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar
    Mixed Modes: From an Asymptotic Description to Data Fitting.” <i>Astronomy and
    Astrophysics</i>, vol. 707, A321, EDP Sciences, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202558023">10.1051/0004-6361/202558023</a>.'
  short: B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics
    707 (2026).
corr_author: '1'
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-04-07T09:01:44Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
- _id: IlCa
- _id: GradSch
doi: 10.1051/0004-6361/202558023
external_id:
  arxiv:
  - '2511.05314 '
file:
- access_level: open_access
  checksum: 560cac19dc70184626b85e71a26ee22e
  content_type: application/pdf
  creator: dernst
  date_created: 2026-04-07T09:00:50Z
  date_updated: 2026-04-07T09:00:50Z
  file_id: '21664'
  file_name: 2026_AstronomyAstrophysics_Liagre.pdf
  file_size: 12287607
  relation: main_file
  success: 1
file_date_updated: 2026-04-07T09:00:50Z
has_accepted_license: '1'
intvolume: '       707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy and Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description
  to data fitting'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21659'
abstract:
- lang: eng
  text: The recent detection of solar equatorial Rossby waves has renewed interest
    in the study of gravito-inertial waves propagating in the convective envelope
    of solar-type stars. In particular, the ability of these envelope gravito-inertial
    modes to couple with those trapped in the radiative interior could open up new
    opportunities for probing the deep-layer dynamics of solar-type stars. The possibility
    for such a coupling to occur is particularly favoured among pre-main-sequence
    (PMS) solar-type stars. Indeed, due to the contraction of the protostellar object,
    they are able to reach high rotation frequencies before nuclear reactions are
    ignited and magnetic braking becomes the driving mechanism for their rotational
    evolution. In this work, we studied the coupling between the envelope inertial
    waves and the radiative interior g modes in PMS stars, focussing on the case of
    prograde dipolar modes. We considered the cases of 0.5 M⊙ and 1 M⊙ PMS models,
    each with three different scenarios of rotational evolution. We show that for
    stars that have formed with a sufficient amount of angular momentum, this coupling
    can occur in frequency ranges that are accessible to space-borne photometry, creating
    inertial dips in the period spacing pattern. Using an asymptotic analysis, we
    characterised the shape of these inertial dips to show that they depend on rotation
    and on the stiffness of the convective-radiative interface.
acknowledgement: 'The authors want to thank the anonymous referee for useful comments.
  SNB acknowledges support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase
  D”. SNB and AFL acknowledge support from the INAF grant MASTODINT. CP thanks the
  Belgian Federal Science Policy Office (BELSPO) for the financial support in the
  framework of the PRODEX Program of the European Space Agency (ESA) under contract
  number 4000141194. S.M acknowledges support from the CNES GOLF-SOHO and PLATO grants
  at CEA/DAp. LB and SM gratefully acknowledge support from the European Research
  Council (ERC) under the Horizon Europe programme (LB: Calcifer; Starting Grant agreement
  N°101165631; SM: 4D-STAR; Synergy Grant agreement N°101071505). While partially
  funded by the European Union, views and opinions expressed are, however, those of
  the authors only and do not necessarily reflect those of the European Union or the
  European Research Council. Neither the European Union nor the granting authority
  can be held responsible for them. The authors acknowledge G. Buldgen, H. Dhouib,
  and M.A. Dupret for fruitful discussions.'
article_number: L16
article_processing_charge: No
article_type: letter_editor
arxiv: 1
author:
- first_name: S. N.
  full_name: Breton, S. N.
  last_name: Breton
- first_name: C.
  full_name: Pezzotti, C.
  last_name: Pezzotti
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: M. P.
  full_name: Di Mauro, M. P.
  last_name: Di Mauro
- first_name: J.
  full_name: Joergensen, J.
  last_name: Joergensen
- first_name: K.
  full_name: Zwintz, K.
  last_name: Zwintz
- first_name: A. F.
  full_name: Lanza, A. F.
  last_name: Lanza
citation:
  ama: Breton SN, Pezzotti C, Mathis S, et al. Core-envelope coupling of gravito-inertial
    waves in pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>.
    2026;707. doi:<a href="https://doi.org/10.1051/0004-6361/202659309">10.1051/0004-6361/202659309</a>
  apa: Breton, S. N., Pezzotti, C., Mathis, S., Bugnet, L. A., Di Mauro, M. P., Joergensen,
    J., … Lanza, A. F. (2026). Core-envelope coupling of gravito-inertial waves in
    pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>. Wiley.
    <a href="https://doi.org/10.1051/0004-6361/202659309">https://doi.org/10.1051/0004-6361/202659309</a>
  chicago: Breton, S. N., C. Pezzotti, S. Mathis, Lisa Annabelle Bugnet, M. P. Di
    Mauro, J. Joergensen, K. Zwintz, and A. F. Lanza. “Core-Envelope Coupling of Gravito-Inertial
    Waves in Pre-Main-Sequence Solar-Type Stars.” <i>Astronomy &#38; Astrophysics</i>.
    Wiley, 2026. <a href="https://doi.org/10.1051/0004-6361/202659309">https://doi.org/10.1051/0004-6361/202659309</a>.
  ieee: S. N. Breton <i>et al.</i>, “Core-envelope coupling of gravito-inertial waves
    in pre-main-sequence solar-type stars,” <i>Astronomy &#38; Astrophysics</i>, vol.
    707. Wiley, 2026.
  ista: Breton SN, Pezzotti C, Mathis S, Bugnet LA, Di Mauro MP, Joergensen J, Zwintz
    K, Lanza AF. 2026. Core-envelope coupling of gravito-inertial waves in pre-main-sequence
    solar-type stars. Astronomy &#38; Astrophysics. 707, L16.
  mla: Breton, S. N., et al. “Core-Envelope Coupling of Gravito-Inertial Waves in
    Pre-Main-Sequence Solar-Type Stars.” <i>Astronomy &#38; Astrophysics</i>, vol.
    707, L16, Wiley, 2026, doi:<a href="https://doi.org/10.1051/0004-6361/202659309">10.1051/0004-6361/202659309</a>.
  short: S.N. Breton, C. Pezzotti, S. Mathis, L.A. Bugnet, M.P. Di Mauro, J. Joergensen,
    K. Zwintz, A.F. Lanza, Astronomy &#38; Astrophysics 707 (2026).
date_created: 2026-04-05T22:01:32Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-04-07T09:23:27Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202659309
external_id:
  arxiv:
  - '2603.01979'
file:
- access_level: open_access
  checksum: a7fd798bf450d67d4166fdf54ff2c70c
  content_type: application/pdf
  creator: dernst
  date_created: 2026-04-07T09:20:02Z
  date_updated: 2026-04-07T09:20:02Z
  file_id: '21666'
  file_name: 2026_AstronomyAstrophysics_Breton.pdf
  file_size: 1535506
  relation: main_file
  success: 1
file_date_updated: 2026-04-07T09:20:02Z
has_accepted_license: '1'
intvolume: '       707'
language:
- iso: eng
month: '03'
oa: 1
oa_version: Published Version
project:
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
  grant_number: '101165631'
  name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: Wiley
quality_controlled: '1'
scopus_import: '1'
status: public
title: Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type
  stars
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21760'
abstract:
- lang: eng
  text: 3I/ATLAS is the third interstellar object discovered to date, following 1I/‘Oumuamua
    and 2I/Borisov. Its unusually high excess velocity and active cometary nature
    make it a key probe of the Galactic population of icy planetesimals. Understanding
    its origin requires its past trajectory through the Galaxy to be traced and the
    possible role of stellar encounters to be assessed, both as a potential origin
    and a perturber to its orbit. We integrated the orbit of 3I/ATLAS backward in
    time for 10 Myr, together with a sample of Gaia DR3 stars with high-quality astrometry
    and radial velocities, to identify close passages within 2 pc. We identify 93
    nominal encounters, 62 of which are significant at the 2σ level. However, none
    of these encounters produced any meaningful perturbation. The strongest perturber
    Gaia DR3 6863591389529611264 at 0.30 pc and with a relative velocity of 35 km
    s−1, imparted only a velocity change of ∣Δv∣  ≃  5  ×  10−4 km s−1 to the orbit
    of 3I/ATLAS. Our results indicate that no stellar flybys within the past 10 Myr
    and 500 pc contained in Gaia DR3 can account for the present trajectory of 3I/ATLAS
    or be associated with its origin. We further show that 3I/ATLAS is kinematically
    consistent with a thin-disk population, despite its large peculiar velocity.
acknowledgement: We thank the anonymous referee for a careful reading of the manuscript
  and for constructive comments that improved the paper. X.P.C. and S.T. thank J.L.
  Gragera-Más and Ylva Götberg for their valuable feedback and comments. X.P.C. acknowledges
  financial support from the Spanish National Programme for the Promotion of Talent
  and its Employability grant PRE2022-104959 cofunded by the European Social Fund.
  S.T. acknowledges the funding from the European Union’s Horizon 2020 research and
  innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413.
  E.V. acknowledges support from the DISCOBOLO project funded by the Spanish Ministerio
  de Ciencia, Innovación y Universidades under grant PID2021-127289NB-I00. A.J.M.
  acknowledges support from the Swedish National Space Agency (Career grant 2023-00146).
  X.P.C. and M.M. acknowledge support from the Spanish Ministerio de Ciencia, Innovaciòn
  y Universidades under grants PID2021122842OB-C22 and PID2024-157964OB-C22; from
  the Xunta de Galicia and the European Union (FEDER Galicia 2021-2027 Program) Ref.
  ED431B 2024/21, ED431B 2024/02, and CITIC ED431G 2023/01. This work has made use
  of data from the European Space Agency (ESA) Gaia mission and processed by the Gaia
  Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided
  by national institutions, particularly the institutions participating in the Gaia
  Multilateral Agreement.
article_number: '146'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: X.
  full_name: Pérez-Couto, X.
  last_name: Pérez-Couto
- first_name: Santiago
  full_name: Torres Rodriguez, Santiago
  id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
  last_name: Torres Rodriguez
  orcid: 0000-0002-3150-8988
- first_name: E.
  full_name: Villaver, E.
  last_name: Villaver
- first_name: A. J.
  full_name: Mustill, A. J.
  last_name: Mustill
- first_name: M.
  full_name: Manteiga, M.
  last_name: Manteiga
citation:
  ama: 'Pérez-Couto X, Torres Rodriguez S, Villaver E, Mustill AJ, Manteiga M. 3I/ATLAS:
    In search of the witnesses to its voyage. <i>The Astrophysical Journal</i>. 2026;1001(2).
    doi:<a href="https://doi.org/10.3847/1538-4357/ae56ff">10.3847/1538-4357/ae56ff</a>'
  apa: 'Pérez-Couto, X., Torres Rodriguez, S., Villaver, E., Mustill, A. J., &#38;
    Manteiga, M. (2026). 3I/ATLAS: In search of the witnesses to its voyage. <i>The
    Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/ae56ff">https://doi.org/10.3847/1538-4357/ae56ff</a>'
  chicago: 'Pérez-Couto, X., Santiago Torres Rodriguez, E. Villaver, A. J. Mustill,
    and M. Manteiga. “3I/ATLAS: In Search of the Witnesses to Its Voyage.” <i>The
    Astrophysical Journal</i>. IOP Publishing, 2026. <a href="https://doi.org/10.3847/1538-4357/ae56ff">https://doi.org/10.3847/1538-4357/ae56ff</a>.'
  ieee: 'X. Pérez-Couto, S. Torres Rodriguez, E. Villaver, A. J. Mustill, and M. Manteiga,
    “3I/ATLAS: In search of the witnesses to its voyage,” <i>The Astrophysical Journal</i>,
    vol. 1001, no. 2. IOP Publishing, 2026.'
  ista: 'Pérez-Couto X, Torres Rodriguez S, Villaver E, Mustill AJ, Manteiga M. 2026.
    3I/ATLAS: In search of the witnesses to its voyage. The Astrophysical Journal.
    1001(2), 146.'
  mla: 'Pérez-Couto, X., et al. “3I/ATLAS: In Search of the Witnesses to Its Voyage.”
    <i>The Astrophysical Journal</i>, vol. 1001, no. 2, 146, IOP Publishing, 2026,
    doi:<a href="https://doi.org/10.3847/1538-4357/ae56ff">10.3847/1538-4357/ae56ff</a>.'
  short: X. Pérez-Couto, S. Torres Rodriguez, E. Villaver, A.J. Mustill, M. Manteiga,
    The Astrophysical Journal 1001 (2026).
date_created: 2026-04-26T22:01:46Z
date_published: 2026-04-20T00:00:00Z
date_updated: 2026-04-28T13:08:39Z
day: '20'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/1538-4357/ae56ff
ec_funded: 1
external_id:
  arxiv:
  - '2509.07678'
file:
- access_level: open_access
  checksum: c3daf49261a9933c079854c38eec316f
  content_type: application/pdf
  creator: dernst
  date_created: 2026-04-28T13:06:00Z
  date_updated: 2026-04-28T13:06:00Z
  file_id: '21773'
  file_name: 2026_AstrophysicalJournal_PerezCouto.pdf
  file_size: 2905627
  relation: main_file
  success: 1
file_date_updated: 2026-04-28T13:06:00Z
has_accepted_license: '1'
intvolume: '      1001'
issue: '2'
language:
- iso: eng
month: '04'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: '3I/ATLAS: In search of the witnesses to its voyage'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 1001
year: '2026'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20350'
abstract:
- lang: eng
  text: "Context. Rotation plays an important role in stellar evolution. However,
    the mechanisms behind the transport of angular momentum in stars at various stages
    of their evolution are not well understood. To improve our understanding of these
    processes, it is necessary to measure and validate the internal rotation profiles
    of stars across different stages of evolution and mass regimes.\r\nAims. Our aim
    is to constrain the internal rotation profile of the 12-M⊙ β Cep pulsator HD 192575
    from the observed pulsational multiplets and the asymmetries of their component
    frequencies.\r\nMethods. We updated the forward asteroseismic modelling of HD
    192575 based on new TESS observations. We inverted the rotation profile from the
    symmetric part of the splittings and computed the multiplet asymmetries due to
    the Coriolis force and stellar deformation, which we treated perturbatively. We
    compared the computed asymmetries with the observed asymmetries.\r\nResults. Our
    new forward asteroseismic modelling is in agreement with previous results but
    with increased uncertainties, partially due to increased frequency precision,
    which required us to relax certain constraints. Ambiguity in the mode identification
    is the main source of the uncertainty, which also affects the inferred rotation
    profiles. Almost all acceptable rotation profiles occur in the regime below 0.4
    d−1 and favour weak radial differential rotation, with a ratio of core to envelope
    rotation of less than 2. We find that the quality of the match between the observed
    and theoretically predicted mode asymmetries is strongly dependent on the mode
    identification and the internal structure of the star.\r\nConclusions. Our results
    offer the first detailed rotation inversion for a β Cep pulsator. They show that
    the rotation profile and the mode asymmetries provide a valuable tool for further
    constraining the evolutionary properties of HD 192575, and in particular the details
    of angular momentum transport in massive stars."
acknowledgement: "The authors appreciated the critical comments from the\r\nreferee,
  which encouraged V.V. to embark upon a new code development\r\nsprint. V.V. gratefully
  acknowledges support from the Research Foundation\r\nFlanders (FWO) under grant
  agreement N◦1156923N (PhD Fellowship) and\r\nN\r\n◦K233724N (Travel grant). D.M.B.
  gratefully acknowledges support from\r\nthe Research Foundation Flanders (FWO; grant
  number: 1286521N), and UK\r\nResearch and Innovation (UKRI) in the form of a Frontier
  Research grant under\r\nthe UK government’s ERC Horizon Europe funding guarantee
  (SYMPHONY;\r\ngrant number: EP/Y031059/1), and a Royal Society University Research
  Fellowship (URF; grant number: URF\\R1\\231631). S.B.D. acknowledges funding from\r\nthe
  European Union’s Horizon 2020 research and innovation programme under\r\nthe Marie
  Skłodowska-Curie grant agreement No 101034413. L.B. gratefully\r\nacknowledges support
  from the European Research Council (ERC) under the\r\nHorizon Europe programme (Calcifer;
  Starting Grant agreement N◦101165631).\r\nS.M. acknowledges support from the PLATO
  CNES grant at CEA/DAp.C.A.\r\nacknowledges financial support from the Research Foundation
  Flanders (FWO)\r\nunder grant K802922N (Sabbatical leave); she is grateful for the
  kind hospitality\r\noffered by CEA/Saclay during her sabbatical work visits in the
  spring of 2023.\r\nThe research leading to these results has received funding from
  the European\r\nResearch Council (ERC) under the Horizon Europe programme (Synergy
  Grant\r\nagreement N◦101071505: 4D-STAR). While funded by the European Union,\r\nviews
  and opinions expressed are however those of the author(s) only and do\r\nnot necessarily
  reflect those of the European Union or the European Research\r\nCouncil. Neither
  the European Union nor the granting authority can be held\r\nresponsible for them.
  The TESS data presented in this paper were obtained from\r\nthe Mikulski Archive
  for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI), which
  is operated by the Association of Universities for\r\nResearch in Astronomy, Inc.,
  under NASA contract NAS5-26555. Support to\r\nMAST for these data is provided by
  the NASA Office of Space Science via grant\r\nNAG5-7584 and by other grants and
  contracts. Funding for the TESS mission\r\nwas provided by the NASA Explorer Program."
article_number: A5
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: V.
  full_name: Vanlaer, V.
  last_name: Vanlaer
- first_name: D. M.
  full_name: Bowman, D. M.
  last_name: Bowman
- first_name: S.
  full_name: Burssens, S.
  last_name: Burssens
- first_name: Srijan B
  full_name: Das, Srijan B
  id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
  last_name: Das
  orcid: 0000-0003-0896-7972
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: C.
  full_name: Aerts, C.
  last_name: Aerts
citation:
  ama: Vanlaer V, Bowman DM, Burssens S, et al. Interior rotation modelling of the
    β Cep pulsator HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>.
    2025;701. doi:<a href="https://doi.org/10.1051/0004-6361/202452885">10.1051/0004-6361/202452885</a>
  apa: Vanlaer, V., Bowman, D. M., Burssens, S., Das, S. B., Bugnet, L. A., Mathis,
    S., &#38; Aerts, C. (2025). Interior rotation modelling of the β Cep pulsator
    HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202452885">https://doi.org/10.1051/0004-6361/202452885</a>
  chicago: Vanlaer, V., D. M. Bowman, S. Burssens, Srijan B Das, Lisa Annabelle Bugnet,
    S. Mathis, and C. Aerts. “Interior Rotation Modelling of the β Cep Pulsator HD
    192575 Including Multiplet Asymmetries.” <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202452885">https://doi.org/10.1051/0004-6361/202452885</a>.
  ieee: V. Vanlaer <i>et al.</i>, “Interior rotation modelling of the β Cep pulsator
    HD 192575 including multiplet asymmetries,” <i>Astronomy &#38; Astrophysics</i>,
    vol. 701. EDP Sciences, 2025.
  ista: Vanlaer V, Bowman DM, Burssens S, Das SB, Bugnet LA, Mathis S, Aerts C. 2025.
    Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet
    asymmetries. Astronomy &#38; Astrophysics. 701, A5.
  mla: Vanlaer, V., et al. “Interior Rotation Modelling of the β Cep Pulsator HD 192575
    Including Multiplet Asymmetries.” <i>Astronomy &#38; Astrophysics</i>, vol. 701,
    A5, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202452885">10.1051/0004-6361/202452885</a>.
  short: V. Vanlaer, D.M. Bowman, S. Burssens, S.B. Das, L.A. Bugnet, S. Mathis, C.
    Aerts, Astronomy &#38; Astrophysics 701 (2025).
date_created: 2025-09-14T22:01:32Z
date_published: 2025-09-01T00:00:00Z
date_updated: 2026-02-16T12:12:53Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202452885
ec_funded: 1
external_id:
  arxiv:
  - '2506.19948'
  isi:
  - '001561561200007'
file:
- access_level: open_access
  checksum: 9ee9f34cf86305602d6cb3e07a1cc1a6
  content_type: application/pdf
  creator: dernst
  date_created: 2025-09-15T06:58:09Z
  date_updated: 2025-09-15T06:58:09Z
  file_id: '20354'
  file_name: 2025_AstronomyAstrophysics_Vanlaer.pdf
  file_size: 3175077
  relation: main_file
  success: 1
file_date_updated: 2025-09-15T06:58:09Z
has_accepted_license: '1'
intvolume: '       701'
isi: 1
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
  grant_number: '101165631'
  name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet
  asymmetries
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 701
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20454'
abstract:
- lang: eng
  text: "Context. γ Dor stars are ideal targets for studies of the innermost dynamical
    properties of stars, due to their rich asteroseismic spectrum of gravity modes.
    Integrating internal magnetism to the picture appears as the next milestone of
    detailed asteroseismic studies, for its prime importance on stellar evolution.
    The inertial dip in prograde dipole modes period-spacing pattern of γ Dors stands
    out as a unique window on the convective core structure and dynamics. Recent studies
    have highlighted the dependence of the dip structure on core density stratification,
    the contrast of the near-core Brunt-Väisälä frequency and rotation rate, as well
    as the core-to-near-core differential rotation. In addition, the effect of envelope
    magnetism has been derived on low-frequency magneto-gravito-inertial waves.\r\n\r\nAims.
    We revisited the inertial dip formation including core and envelope magnetism,
    and explored the probing power of this feature on dynamo-generated core fields.\r\n\r\nMethods.
    We considered as a first step a toroidal magnetic field with a bi-layer (core
    and envelope) Alfvén frequency. This configuration allowed us to revisit the coupling
    problem using our knowledge on both core magneto-inertial modes and envelope magneto-gravito-inertial
    modes. Using this configuration, we were able to stay in an analytical framework
    to exhibit the magnetic effects on the inertial dip shape and location. This configuration
    allowed a laboratory to be set up that moves us towards the comprehension of magnetic
    effects on the dip structure.\r\n\r\nResults. We show a shift of the inertial
    dip towards lower spin parameter values and a thinner dip with increasing core
    magnetic field’s strength, quite similar to the signature of differential rotation.
    The magnetic effects become sizeable when the ratio of the magnetic to the Coriolis
    effects is high enough. We explored the potential degeneracy of the magnetic effects
    with differential rotation. We studied the detectability of core magnetism, considering
    both observational constraints on the periods of the modes and potential gravito-inertial
    mode suppression."
acknowledgement: 'We thank the referee for their comments and suggestions which allowed
  us to improve the quality of this manuscript. L. Barrault and L. Bugnet gratefully
  acknowledge support from the European Research Council (ERC) under the Horizon Europe
  programme (Calcifer; Starting Grant agreement N°101165631). S. Mathis acknowledges
  support from the PLATO CNES grant at CEA/DAp. S. Mathis and J.S.G. Mombarg acknowledge
  support from the European Research Council through HORIZON ERC SyG Grant 4D-STAR
  101071505. While partially funded by the European Union, views and opinions expressed
  are however those of the authors only and do not necessarily reflect those of the
  European Union or the European Research Council. Neither the European Union nor
  the granting authority can be held responsible for them. L. Barrault thanks T. Van
  Reeth and C. Aerts for their invaluable teachings. The authors thank also the members
  of the Asteroseismology and Stellar Dynamics group of the Institute of Science and
  Technology Austria (ISTA) for very useful discussion: A. Cristea, L. Einramhof,
  K. M. Smith, S. Torres.'
article_number: A253
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Lucas
  full_name: Barrault, Lucas
  id: 4471a8fd-32c1-11ee-a9a4-fb670d398f64
  last_name: Barrault
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: J. S.G.
  full_name: Mombarg, J. S.G.
  last_name: Mombarg
citation:
  ama: 'Barrault L, Bugnet LA, Mathis S, Mombarg JSG. Exploring the probing power
    of γ Dor’s inertial dip for core magnetism: The case of a toroidal field. <i>Astronomy
    &#38; Astrophysics</i>. 2025;701. doi:<a href="https://doi.org/10.1051/0004-6361/202555213">10.1051/0004-6361/202555213</a>'
  apa: 'Barrault, L., Bugnet, L. A., Mathis, S., &#38; Mombarg, J. S. G. (2025). Exploring
    the probing power of γ Dor’s inertial dip for core magnetism: The case of a toroidal
    field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202555213">https://doi.org/10.1051/0004-6361/202555213</a>'
  chicago: 'Barrault, Lucas, Lisa Annabelle Bugnet, S. Mathis, and J. S.G. Mombarg.
    “Exploring the Probing Power of γ Dor’s Inertial Dip for Core Magnetism: The Case
    of a Toroidal Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025.
    <a href="https://doi.org/10.1051/0004-6361/202555213">https://doi.org/10.1051/0004-6361/202555213</a>.'
  ieee: 'L. Barrault, L. A. Bugnet, S. Mathis, and J. S. G. Mombarg, “Exploring the
    probing power of γ Dor’s inertial dip for core magnetism: The case of a toroidal
    field,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.'
  ista: 'Barrault L, Bugnet LA, Mathis S, Mombarg JSG. 2025. Exploring the probing
    power of γ Dor’s inertial dip for core magnetism: The case of a toroidal field.
    Astronomy &#38; Astrophysics. 701, A253.'
  mla: 'Barrault, Lucas, et al. “Exploring the Probing Power of γ Dor’s Inertial Dip
    for Core Magnetism: The Case of a Toroidal Field.” <i>Astronomy &#38; Astrophysics</i>,
    vol. 701, A253, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202555213">10.1051/0004-6361/202555213</a>.'
  short: L. Barrault, L.A. Bugnet, S. Mathis, J.S.G. Mombarg, Astronomy &#38; Astrophysics
    701 (2025).
corr_author: '1'
date_created: 2025-10-12T22:01:26Z
date_published: 2025-09-01T00:00:00Z
date_updated: 2026-02-19T09:32:04Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
- _id: GradSch
doi: 10.1051/0004-6361/202555213
external_id:
  arxiv:
  - '2507.00308'
  isi:
  - '001585834500002'
file:
- access_level: open_access
  checksum: 2c209b33119af4a251bab4a418a21075
  content_type: application/pdf
  creator: dernst
  date_created: 2025-10-13T07:05:55Z
  date_updated: 2025-10-13T07:05:55Z
  file_id: '20459'
  file_name: 2025_AstronomyAstrophysics_BarraultL.pdf
  file_size: 2503149
  relation: main_file
  success: 1
file_date_updated: 2025-10-13T07:05:55Z
has_accepted_license: '1'
intvolume: '       701'
isi: 1
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
project:
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
  grant_number: '101165631'
  name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Exploring the probing power of γ Dor''s inertial dip for core magnetism: The
  case of a toroidal field'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 701
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '18984'
abstract:
- lang: eng
  text: Although planets have been found orbiting binary systems, whether they can
    survive binary interactions is debated. While the tightest-orbit binaries should
    host the most dynamically stable and long-lived circumbinary planetary systems,
    they are also the systems that are expected to experience mass transfer, common
    envelope evolution, or stellar mergers. In this study, we explore the effect of
    stable non-conservative mass transfer on the dynamical evolution of circumbinary
    planets. We present a new script that seamlessly integrates binary evolution data
    from the 1D binary stellar evolution code MESA into the N-body simulation code
    REBOUND. This integration framework enables a comprehensive examination of the
    dynamical evolution of circumbinary planets orbiting mass-transferring binaries,
    while simultaneously accounting for the detailed stellar structure evolution.
    In addition, we introduce a recalibration method to mitigate numerical errors
    from updates of binary properties during the system's dynamical evolution. We
    construct a reference binary model in which a 2.21M⊙ star loses its hydrogen-rich
    envelope through non-conservative mass transfer to the 1.76M⊙ companion star,
    creating a 0.38M⊙ subdwarf. We find the tightest stable orbital separation for
    circumbinary planets to be ≃2.5 times the binary separation after mass transfer.
    Accounting for tides by using the interior stellar structure, we find that tidal
    effects become apparent after the rapid mass transfer phase and start to fade
    away during the latter stage of the slow mass transfer phase. Our research provides
    a new framework for exploring circumbinary planet dynamics in interacting binary
    systems.
acknowledgement: We thank the participants of the 2023 Kavli Summer Program in Astrophysics,
  hosted by the Max Planck Institute for Astrophysics and funded by the Kavli Foundation.
  In particular, Holly Preece, Selma de Mink, and Stephen Justham for their feedback
  and comments on our work. ZX acknowledges support from the China Scholarship Council
  (CSC). ST acknowledges the funding from the European Union’s Horizon 2020 research
  and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101034413.
  AAT acknowledges support from the Horizon Europe research and innovation programmes
  under the Marie Skłodowska-Curie grant agreement no. 101103134.
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zepei
  full_name: Xing, Zepei
  last_name: Xing
- first_name: Santiago
  full_name: Torres Rodriguez, Santiago
  id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
  last_name: Torres Rodriguez
  orcid: 0000-0002-3150-8988
- first_name: Ylva Louise Linsdotter
  full_name: Götberg, Ylva Louise Linsdotter
  id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
  last_name: Götberg
  orcid: 0000-0002-6960-6911
- first_name: Alessandro A.
  full_name: Trani, Alessandro A.
  last_name: Trani
- first_name: Valeriya
  full_name: Korol, Valeriya
  last_name: Korol
- first_name: Jorge
  full_name: Cuadra, Jorge
  last_name: Cuadra
citation:
  ama: 'Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. Combining
    REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries.
    <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(1):285-292.
    doi:<a href="https://doi.org/10.1093/mnras/stae2820">10.1093/mnras/stae2820</a>'
  apa: 'Xing, Z., Torres Rodriguez, S., Götberg, Y. L. L., Trani, A. A., Korol, V.,
    &#38; Cuadra, J. (2025). Combining REBOUND and MESA: Dynamical evolution of planets
    orbiting interacting binaries. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stae2820">https://doi.org/10.1093/mnras/stae2820</a>'
  chicago: 'Xing, Zepei, Santiago Torres Rodriguez, Ylva Louise Linsdotter Götberg,
    Alessandro A. Trani, Valeriya Korol, and Jorge Cuadra. “Combining REBOUND and
    MESA: Dynamical Evolution of Planets Orbiting Interacting Binaries.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025.
    <a href="https://doi.org/10.1093/mnras/stae2820">https://doi.org/10.1093/mnras/stae2820</a>.'
  ieee: 'Z. Xing, S. Torres Rodriguez, Y. L. L. Götberg, A. A. Trani, V. Korol, and
    J. Cuadra, “Combining REBOUND and MESA: Dynamical evolution of planets orbiting
    interacting binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 537, no. 1. Oxford University Press, pp. 285–292, 2025.'
  ista: 'Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. 2025.
    Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting
    binaries. Monthly Notices of the Royal Astronomical Society. 537(1), 285–292.'
  mla: 'Xing, Zepei, et al. “Combining REBOUND and MESA: Dynamical Evolution of Planets
    Orbiting Interacting Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 537, no. 1, Oxford University Press, 2025, pp. 285–92, doi:<a href="https://doi.org/10.1093/mnras/stae2820">10.1093/mnras/stae2820</a>.'
  short: Z. Xing, S. Torres Rodriguez, Y.L.L. Götberg, A.A. Trani, V. Korol, J. Cuadra,
    Monthly Notices of the Royal Astronomical Society 537 (2025) 285–292.
date_created: 2025-02-02T23:01:53Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2025-12-30T07:25:37Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
- _id: LiBu
doi: 10.1093/mnras/stae2820
ec_funded: 1
external_id:
  arxiv:
  - '2410.19695'
  isi:
  - '001400731500001'
file:
- access_level: open_access
  checksum: 49fb4fe69f487d36169ccea60acbeccc
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  creator: dernst
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  date_updated: 2025-12-30T07:24:34Z
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  file_name: 2025_MonthlyNoticesRAS_Xing.pdf
  file_size: 2974244
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file_date_updated: 2025-12-30T07:24:34Z
has_accepted_license: '1'
intvolume: '       537'
isi: 1
issue: '1'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
page: 285-292
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting
  binaries'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 537
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19283'
abstract:
- lang: eng
  text: "Context. The presence of dips in the gravity mode period spacing versus period
    diagram of γ Doradus stars is now well established thanks to recent asteroseismic
    studies. Such Lorentzian-shaped inertial dips arise from the interaction of gravito-inertial
    modes in the radiative envelope of intermediate-mass main sequence stars with
    pure inertial modes in their convective core, and allow us to study stellar internal
    properties. This window onto stellar internal dynamics is extremely valuable in
    the context of the understanding of angular-momentum transport inside stars, as
    it allows us to probe rotation in their core.\r\n\r\nAims. We investigate the
    signature and the detectability of a differential rotation between the convective
    core and the near-core region inside γ Doradus stars from the properties of inertial
    dips.\r\n\r\nMethods. We studied the coupling between gravito-inertial modes in
    the radiative zone and pure inertial modes in the convective core in the sub-inertial
    regime, allowing for a two-zone differential rotation from the two sides of the
    core-to-envelope boundary. We solved the coupling equation numerically and matched
    the result to an analytical derivation of the Lorentzian dip properties. We then
    used typical values of measured near-core rotation and buoyancy travel time to
    infer ranges of parameters for which differential core to near-core rotation would
    be detectable in current Kepler data.\r\n\r\nResults. We show that increasing
    the convective core rotation with respect to the near-core rotation leads to a
    shift of the period of the observed dip to lower periods. In addition, the dip
    gets deeper and thinner as the convective core rotation increases. We demonstrate
    that such a signature is detectable in Kepler data, given appropriate dip-parameter
    ranges and near-core structural properties.\r\n\r\nConclusions. Studying the dip
    properties in asteroseismic data thus allows us to access core to near-core radial
    differential rotation and to better understand the transport of angular momentum
    at convective–radiative interfaces in intermediate-mass main sequence stars."
acknowledgement: 'We thank the referee for very constructive and detailed comments
  that led to an improvement of the quality of our study. L.B. and L.B. gratefully
  acknowledge support from the European Research Council (ERC) under the Horizon Europe
  programme (Calcifer; Starting Grant agreement N°101165631). S. Mathis acknowledges
  support from the PLATO CNES grant at CEA/DAp and from the European Research Council
  through HORIZON ERC SyG Grant 4D-STAR 101071505. While partially funded by the European
  Union, views and opinions expressed are however those of the author only and do
  not necessarily reflect those of the European Union or the European Research Council.
  Neither the European Union nor the granting authority can be held responsible for
  them. L. Barrault thanks the members of the asteroseismology group of the Institute
  of Astronomy (IvS) of KU Leuven, in particular T. Van Reeth, M. Vanrespaille, Z.
  Guo and C. Aerts, for their warm welcome during a work visit in Spring 2024, and
  very insightful input on the present study. The authors thank also the members of
  the Asteroseismology and Stellar Dynamics group of the Institute of Science and
  Technology Austria (ISTA) for very useful discussion: K. M. Smith, L. Einramhof,
  S. Torres and A. Cristea.'
article_number: A225
article_processing_charge: Yes
article_type: original
author:
- first_name: Lucas
  full_name: Barrault, Lucas
  id: 4471a8fd-32c1-11ee-a9a4-fb670d398f64
  last_name: Barrault
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
citation:
  ama: Barrault L, Mathis S, Bugnet LA. Constraining differential rotation in γ Doradus
    stars from the properties of inertial dips. <i>Astronomy &#38; Astrophysics</i>.
    2025;694. doi:<a href="https://doi.org/10.1051/0004-6361/202451541">10.1051/0004-6361/202451541</a>
  apa: Barrault, L., Mathis, S., &#38; Bugnet, L. A. (2025). Constraining differential
    rotation in γ Doradus stars from the properties of inertial dips. <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202451541">https://doi.org/10.1051/0004-6361/202451541</a>
  chicago: Barrault, Lucas, S. Mathis, and Lisa Annabelle Bugnet. “Constraining Differential
    Rotation in γ Doradus Stars from the Properties of Inertial Dips.” <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202451541">https://doi.org/10.1051/0004-6361/202451541</a>.
  ieee: L. Barrault, S. Mathis, and L. A. Bugnet, “Constraining differential rotation
    in γ Doradus stars from the properties of inertial dips,” <i>Astronomy &#38; Astrophysics</i>,
    vol. 694. EDP Sciences, 2025.
  ista: Barrault L, Mathis S, Bugnet LA. 2025. Constraining differential rotation
    in γ Doradus stars from the properties of inertial dips. Astronomy &#38; Astrophysics.
    694, A225.
  mla: Barrault, Lucas, et al. “Constraining Differential Rotation in γ Doradus Stars
    from the Properties of Inertial Dips.” <i>Astronomy &#38; Astrophysics</i>, vol.
    694, A225, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202451541">10.1051/0004-6361/202451541</a>.
  short: L. Barrault, S. Mathis, L.A. Bugnet, Astronomy &#38; Astrophysics 694 (2025).
corr_author: '1'
date_created: 2025-03-02T23:01:53Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2026-02-16T12:09:14Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202451541
external_id:
  isi:
  - '001424452400025'
file:
- access_level: open_access
  checksum: 568a5e5951f20483663df145a780fc3d
  content_type: application/pdf
  creator: dernst
  date_created: 2025-03-04T09:57:03Z
  date_updated: 2025-03-04T09:57:03Z
  file_id: '19288'
  file_name: 2025_AstronomyAstrophysics_Barrault.pdf
  file_size: 7438476
  relation: main_file
  success: 1
file_date_updated: 2025-03-04T09:57:03Z
has_accepted_license: '1'
intvolume: '       694'
isi: 1
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
project:
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
  grant_number: '101165631'
  name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Constraining differential rotation in γ Doradus stars from the properties of
  inertial dips
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 694
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '19405'
abstract:
- lang: eng
  text: "In the third APOKASC catalog, we present data for the complete sample of
    15,808 evolved stars with APOGEE spectroscopic parameters and Kepler asteroseismology.
    We used 10 independent asteroseismic analysis techniques and anchor our system
    on fundamental radii derived from Gaia L and spectroscopic Teff. We provide evolutionary
    state, asteroseismic surface gravity, mass, radius, age, and the data used to
    derive them for 12,418 stars. This includes 10,036 exceptionally precise measurements,
    with median fractional uncertainties in \r\nvmax, Δν, mass, radius, and age of
    0.6%, 0.6%, 3.8%, 1.8%, and 11.1%, respectively. We provide more limited data
    for 1624 additional stars that either have lower-quality data or are outside of
    our primary calibration domain. Using lower red giant branch (RGB) stars, we find
    a median age for the chemical thick disk of 9.14 ± 0.05(ran) ± 0.9(sys) Gyr with
    an age dispersion of 1.1 Gyr, consistent with our error model. We calibrate our
    red clump (RC) mass loss to derive an age consistent with the lower RGB and provide
    asymptotic GB and RGB ages for luminous stars. We also find a sharp upper-age
    boundary in the chemical thin disk. We find that scaling relations are precise
    and accurate on the lower RGB and RC, but they become more model dependent for
    more luminous giants and break down at the tip of the RGB. We recommend the use
    of multiple methods, calibration to a fundamental scale, and the use of stellar
    models to interpret frequency spacings."
acknowledgement: "We thank the anonymous referee for providing constructive comments
  that improved the paper. This paper includes data collected by the Kepler mission
  and obtained from the MAST data archive at the Space Telescope Science Institute
  (STScI). Funding for the Kepler mission is provided by the NASA Science Mission
  Directorate. STScI is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-26555. M.H.P. acknowledges support from
  NASA grants 80NSSC24K0637 and 80NSSC18K1582. M.H.P., J.T., and P.M.F. acknowledge
  that part of this work was performed at the Aspen Center for Physics, which is supported
  by National Science Foundation grant PHY-1607611. M.H.P. acknowledges support from
  the Fundación Occident and the Instituto de Astrofísica de Canarias under the Visiting
  Researcher Programme 2022-2025 agreed between both institutions. A.S. acknowledges
  support by the Spanish Ministry of Science, Innovation and Universities through
  the grant PID2023-149918NB-I00 and the program Unidad de Excelencia Marìa de Maeztu
  CEX2020-001058-M, and by Generalitat de Catalunya through grant 2021-SGR-1526. S.B.
  acknowledges NSF grant AST-2205026. P.G.B. acknowledges support by the Spanish Ministry
  of Science and Innovation with the Ramón y Cajal fellowship Nos. RYC-2021-033137-I
  and MRR4032204. D.S. is supported by the Australian Research Council (DP190100666).
  P.G.B., D.G.R., and R.A.G. acknowledge support from the Spanish Ministry of Science
  and Innovation from grant No. PID2023-146453NB-100 (PLAtoSOnG). M.V. acknowledges
  support from NASA grant 80NSSC18K1582 and funding from the European Research Council
  (ERC) under the European Union's Horizon 2020 research and innovation program (grant
  agreement No. 101019653). T.C.B. acknowledges partial support for this work from
  grant PHY 14-30152; Physics Frontier Center/JINA Center for the Evolution of the
  Elements (JINA-CEE), and OISE-1927130: The International Research Network for Nuclear
  Astrophysics (IReNA), awarded by the US National Science Foundation. The research
  leading to the presented results has received funding from the ERC Consolidator
  Grant DipolarSound (grant agreement No. 101000296). P.F. and T.S. acknowledges support
  from the National Science Foundation Astronomy and Astrophysics grants AST-1715662
  and AST-2206541. S.M. acknowledges support by the Spanish Ministry of Science and
  Innovation with the Ramon y Cajal fellowship Nos. RYC-2015-17697, PID2019-107061GB-C66,
  and PID2023-149439NB-C41, and through AEI under the Severo Ochoa Centres of Excellence
  Programme 2020–2023 (CEX2019-000920-S). S.M. and D.G.R. acknowledge support from
  the Spanish Ministry of Science and Innovation (MICINN) from grant No. PID2019-107187GB-I00.
  D.G.R. acknowledges support from the Spanish Ministry of Science and Innovation
  (MICINN) with the Juan de la Cierva program under contract JDC2022-049054-I. L.B.
  gratefully acknowledges support from the European Research Council (ERC) under the
  Horizon Europe program (Calcifer; Starting grant agreement No. 101165631). A.R.G.S.
  acknowledges the support from the FCT through national funds and FEDER through COMPETE2020
  (UIDB/04434/2020, UIDP/04434/2020, and 2022.03993.PTDC) and the support from the
  FCT through work contract No. 2020.02480.CEECIND/CP1631/CT0001.\r\n\r\nFunding for
  the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation,
  the U.S. Department of Energy Office of Science, and the Participating Institutions.
  SDSS acknowledges support and resources from the Center for High-Performance Computing
  at the University of Utah. The SDSS website is www.sdss4.org.\r\n\r\nSDSS is managed
  by the Astrophysical Research Consortium for the Participating Institutions of the
  SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution
  for Science, Carnegie Mellon University, Center for Astrophysics—Harvard & Smithsonian
  (CfA), the Chilean Participation Group, the French Participation Group, Instituto
  de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the
  Physics and Mathematics of the Universe (IPMU)/University of Tokyo, the Korean Participation
  Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam
  (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut
  für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik
  (MPE), National Astronomical Observatories of China, New Mexico State University,
  New York University, University of Notre Dame, Observatório Nacional/MCTI, The Ohio
  State University, Pennsylvania State University, Shanghai Astronomical Observatory,
  United Kingdom Participation Group, Universidad Nacional Autónoma de México, University
  of Arizona, University of Colorado Boulder, University of Oxford, University of
  Portsmouth, University of Utah, University of Virginia, University of Washington,
  University of Wisconsin, Vanderbilt University, and Yale University."
article_number: '69'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Marc H.
  full_name: Pinsonneault, Marc H.
  last_name: Pinsonneault
- first_name: Joel C.
  full_name: Zinn, Joel C.
  last_name: Zinn
- first_name: Jamie
  full_name: Tayar, Jamie
  last_name: Tayar
- first_name: Aldo
  full_name: Serenelli, Aldo
  last_name: Serenelli
- first_name: Rafael A.
  full_name: García, Rafael A.
  last_name: García
- first_name: Savita
  full_name: Mathur, Savita
  last_name: Mathur
- first_name: Mathieu
  full_name: Vrard, Mathieu
  last_name: Vrard
- first_name: Yvonne P.
  full_name: Elsworth, Yvonne P.
  last_name: Elsworth
- first_name: Benoit
  full_name: Mosser, Benoit
  last_name: Mosser
- first_name: Dennis
  full_name: Stello, Dennis
  last_name: Stello
- first_name: Keaton J.
  full_name: Bell, Keaton J.
  last_name: Bell
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: Enrico
  full_name: Corsaro, Enrico
  last_name: Corsaro
- first_name: Patrick
  full_name: Gaulme, Patrick
  last_name: Gaulme
- first_name: Saskia
  full_name: Hekker, Saskia
  last_name: Hekker
- first_name: Marc
  full_name: Hon, Marc
  last_name: Hon
- first_name: Daniel
  full_name: Huber, Daniel
  last_name: Huber
- first_name: Thomas
  full_name: Kallinger, Thomas
  last_name: Kallinger
- first_name: Kaili
  full_name: Cao, Kaili
  last_name: Cao
- first_name: Jennifer A.
  full_name: Johnson, Jennifer A.
  last_name: Johnson
- first_name: Bastien
  full_name: Liagre, Bastien
  last_name: Liagre
- first_name: Rachel A.
  full_name: Patton, Rachel A.
  last_name: Patton
- first_name: Ângela R.G.
  full_name: Santos, Ângela R.G.
  last_name: Santos
- first_name: Sarbani
  full_name: Basu, Sarbani
  last_name: Basu
- first_name: Paul G.
  full_name: Beck, Paul G.
  last_name: Beck
- first_name: Timothy C.
  full_name: Beers, Timothy C.
  last_name: Beers
- first_name: William J.
  full_name: Chaplin, William J.
  last_name: Chaplin
- first_name: Katia
  full_name: Cunha, Katia
  last_name: Cunha
- first_name: Peter M.
  full_name: Frinchaboy, Peter M.
  last_name: Frinchaboy
- first_name: Léo
  full_name: Girardi, Léo
  last_name: Girardi
- first_name: Diego
  full_name: Godoy-Rivera, Diego
  last_name: Godoy-Rivera
- first_name: Jon A.
  full_name: Holtzman, Jon A.
  last_name: Holtzman
- first_name: Henrik
  full_name: Jönsson, Henrik
  last_name: Jönsson
- first_name: Szabolcs
  full_name: Mészáros, Szabolcs
  last_name: Mészáros
- first_name: Claudia
  full_name: Reyes, Claudia
  last_name: Reyes
- first_name: Hans Walter
  full_name: Rix, Hans Walter
  last_name: Rix
- first_name: Matthew
  full_name: Shetrone, Matthew
  last_name: Shetrone
- first_name: Verne V.
  full_name: Smith, Verne V.
  last_name: Smith
- first_name: Taylor
  full_name: Spoo, Taylor
  last_name: Spoo
- first_name: Keivan G.
  full_name: Stassun, Keivan G.
  last_name: Stassun
- first_name: Ji
  full_name: Wang, Ji
  last_name: Wang
citation:
  ama: 'Pinsonneault MH, Zinn JC, Tayar J, et al. APOKASC-3: The third joint spectroscopic
    and asteroseismic catalog for evolved stars in the Kepler fields. <i>Astrophysical
    Journal, Supplement Series</i>. 2025;276(2). doi:<a href="https://doi.org/10.3847/1538-4365/ad9fef">10.3847/1538-4365/ad9fef</a>'
  apa: 'Pinsonneault, M. H., Zinn, J. C., Tayar, J., Serenelli, A., García, R. A.,
    Mathur, S., … Wang, J. (2025). APOKASC-3: The third joint spectroscopic and asteroseismic
    catalog for evolved stars in the Kepler fields. <i>Astrophysical Journal, Supplement
    Series</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4365/ad9fef">https://doi.org/10.3847/1538-4365/ad9fef</a>'
  chicago: 'Pinsonneault, Marc H., Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael
    A. García, Savita Mathur, Mathieu Vrard, et al. “APOKASC-3: The Third Joint Spectroscopic
    and Asteroseismic Catalog for Evolved Stars in the Kepler Fields.” <i>Astrophysical
    Journal, Supplement Series</i>. IOP Publishing, 2025. <a href="https://doi.org/10.3847/1538-4365/ad9fef">https://doi.org/10.3847/1538-4365/ad9fef</a>.'
  ieee: 'M. H. Pinsonneault <i>et al.</i>, “APOKASC-3: The third joint spectroscopic
    and asteroseismic catalog for evolved stars in the Kepler fields,” <i>Astrophysical
    Journal, Supplement Series</i>, vol. 276, no. 2. IOP Publishing, 2025.'
  ista: 'Pinsonneault MH, Zinn JC, Tayar J, Serenelli A, García RA, Mathur S, Vrard
    M, Elsworth YP, Mosser B, Stello D, Bell KJ, Bugnet LA, Corsaro E, Gaulme P, Hekker
    S, Hon M, Huber D, Kallinger T, Cao K, Johnson JA, Liagre B, Patton RA, Santos
    ÂRG, Basu S, Beck PG, Beers TC, Chaplin WJ, Cunha K, Frinchaboy PM, Girardi L,
    Godoy-Rivera D, Holtzman JA, Jönsson H, Mészáros S, Reyes C, Rix HW, Shetrone
    M, Smith VV, Spoo T, Stassun KG, Wang J. 2025. APOKASC-3: The third joint spectroscopic
    and asteroseismic catalog for evolved stars in the Kepler fields. Astrophysical
    Journal, Supplement Series. 276(2), 69.'
  mla: 'Pinsonneault, Marc H., et al. “APOKASC-3: The Third Joint Spectroscopic and
    Asteroseismic Catalog for Evolved Stars in the Kepler Fields.” <i>Astrophysical
    Journal, Supplement Series</i>, vol. 276, no. 2, 69, IOP Publishing, 2025, doi:<a
    href="https://doi.org/10.3847/1538-4365/ad9fef">10.3847/1538-4365/ad9fef</a>.'
  short: M.H. Pinsonneault, J.C. Zinn, J. Tayar, A. Serenelli, R.A. García, S. Mathur,
    M. Vrard, Y.P. Elsworth, B. Mosser, D. Stello, K.J. Bell, L.A. Bugnet, E. Corsaro,
    P. Gaulme, S. Hekker, M. Hon, D. Huber, T. Kallinger, K. Cao, J.A. Johnson, B.
    Liagre, R.A. Patton, Â.R.G. Santos, S. Basu, P.G. Beck, T.C. Beers, W.J. Chaplin,
    K. Cunha, P.M. Frinchaboy, L. Girardi, D. Godoy-Rivera, J.A. Holtzman, H. Jönsson,
    S. Mészáros, C. Reyes, H.W. Rix, M. Shetrone, V.V. Smith, T. Spoo, K.G. Stassun,
    J. Wang, Astrophysical Journal, Supplement Series 276 (2025).
date_created: 2025-03-16T23:01:24Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2025-09-30T11:03:01Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/1538-4365/ad9fef
external_id:
  arxiv:
  - '2410.00102'
  isi:
  - '001414132600001'
file:
- access_level: open_access
  checksum: a01a6645c6cb0b5cc75490f3339a2244
  content_type: application/pdf
  creator: dernst
  date_created: 2025-03-17T10:40:41Z
  date_updated: 2025-03-17T10:40:41Z
  file_id: '19414'
  file_name: 2025_AstrophysicalJourSuppl_Pinsonneault.pdf
  file_size: 4993506
  relation: main_file
  success: 1
file_date_updated: 2025-03-17T10:40:41Z
has_accepted_license: '1'
intvolume: '       276'
isi: 1
issue: '2'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal, Supplement Series
publication_identifier:
  issn:
  - 0067-0049
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'APOKASC-3: The third joint spectroscopic and asteroseismic catalog for evolved
  stars in the Kepler fields'
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 276
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20930'
abstract:
- lang: eng
  text: "Context. Beta Pictoris is an A-type star that hosts a complex planetary system
    with two massive gas giants and a prominent debris disc. Variable absorption lines
    in its stellar spectrum have been interpreted as signatures of exocomets – comet-like
    bodies transiting the star. Stellar flybys can gravitationally perturb objects
    in the outer comet reservoir, altering their orbits and potentially injecting
    them into the inner system, thereby triggering exocomet showers.\r\nAims. We assessed
    the contribution of stellar flybys to the observed exocomet activity by reconstructing
    the stellar encounter history of β Pictoris in the past and future.\r\nMethods.
    We used Gaia DR3 data, supplemented with radial velocities from complementary
    spectroscopic surveys, to compile a catalogue of stars currently within 80 pc
    of β Pictoris. Their orbits were integrated backwards and forwards in time in
    an axisymmetric Galactic potential (via the GALA package) to identify encounters
    within 2 pc of the system.\r\nResults. We identified 99 416 stars currently within
    80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including
    the eight components of five binaries) encounter β Pictoris within 2 pc between
    –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories
    also pass within 2 pc. We estimated the sample to be more than 60% complete within
    0.5 Myr of today.\r\nConclusions. Despite β Pictoris being the eponym of its famous
    moving group, none of the identified encounters involved its moving group members;
    all are unrelated field stars. We found no encounter capable of shaping the observed
    disc structures, although stellar flybys may contribute to the long-term evolution
    of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction
    of the β Pictoris encounter history to date and provides a robust foundation for
    future dynamical simulations."
acknowledgement: We thank the referee for their suggestions and comments, which helped
  us improve the quality and clarity of the paper. JLGM and EV acknowledge the support
  from the Spanish Ministry of Science and Innovation/State Agency of Research (MCIN/AEI)
  under the grant PID2021-127289-NB-I00. ST acknowledges the funding from the European
  Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie
  grant agreement No. 101034413. AJM acknowledges support from the Swedish National
  Space Agency (Career Grant 2023-00146) and from the Swedish Research Council (Project
  Grant 2022-04043). JLGM also sincerely thanks AMP for his careful final reading
  of this manuscript. This work has made use of data from the European Space Agency
  (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data
  Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided
  by national institutions, in particular the institutions participating in the Gaia
  Multilateral Agreement. We acknowledge the use of the public data products from
  RAVE (https://www.rave-survey.org), GALAH (https://galah-survey.org), APOGEE ((https://www.sdss.org)
  and LAMOST (http://www.lamost.org) surveys. This research has also made use of the
  SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg,
  France, as well as the NASA Astrophysics Data System Bibliographic Services and
  the arXiv pre-print server operated by Cornell University. Computational analyses
  in this work relied extensively on the NumPy and SciPy libraries for numerical computing,
  matplotlib and seaborn for data visualization, and the Gala package for Galactic
  dynamics. This work also made use of Astropy, a community-developed core PYTHON
  package and an ecosystem of tools and resources for astronomy. We thank the developers
  and maintainers of these open-source resources for their invaluable contributions
  to the astronomical community.
article_number: A237
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J. L.
  full_name: Gragera-Más, J. L.
  last_name: Gragera-Más
- first_name: Santiago
  full_name: Torres Rodriguez, Santiago
  id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
  last_name: Torres Rodriguez
  orcid: 0000-0002-3150-8988
- first_name: A. J.
  full_name: Mustill, A. J.
  last_name: Mustill
- first_name: E.
  full_name: Villaver, E.
  last_name: Villaver
citation:
  ama: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. A kinematic history
    of stellar encounters with Beta Pictoris. <i>Astronomy &#38; Astrophysics</i>.
    2025;704. doi:<a href="https://doi.org/10.1051/0004-6361/202555940">10.1051/0004-6361/202555940</a>
  apa: Gragera-Más, J. L., Torres Rodriguez, S., Mustill, A. J., &#38; Villaver, E.
    (2025). A kinematic history of stellar encounters with Beta Pictoris. <i>Astronomy
    &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202555940">https://doi.org/10.1051/0004-6361/202555940</a>
  chicago: Gragera-Más, J. L., Santiago Torres Rodriguez, A. J. Mustill, and E. Villaver.
    “A Kinematic History of Stellar Encounters with Beta Pictoris.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202555940">https://doi.org/10.1051/0004-6361/202555940</a>.
  ieee: J. L. Gragera-Más, S. Torres Rodriguez, A. J. Mustill, and E. Villaver, “A
    kinematic history of stellar encounters with Beta Pictoris,” <i>Astronomy &#38;
    Astrophysics</i>, vol. 704. EDP Sciences, 2025.
  ista: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. 2025. A kinematic
    history of stellar encounters with Beta Pictoris. Astronomy &#38; Astrophysics.
    704, A237.
  mla: Gragera-Más, J. L., et al. “A Kinematic History of Stellar Encounters with
    Beta Pictoris.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A237, EDP Sciences,
    2025, doi:<a href="https://doi.org/10.1051/0004-6361/202555940">10.1051/0004-6361/202555940</a>.
  short: J.L. Gragera-Más, S. Torres Rodriguez, A.J. Mustill, E. Villaver, Astronomy
    &#38; Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:34Z
date_published: 2025-12-01T00:00:00Z
date_updated: 2026-02-16T12:15:07Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202555940
ec_funded: 1
external_id:
  arxiv:
  - '2510.02509'
file:
- access_level: open_access
  checksum: 2fb4d5a1603043aa7931a31f2c180877
  content_type: application/pdf
  creator: dernst
  date_created: 2026-01-05T11:06:16Z
  date_updated: 2026-01-05T11:06:16Z
  file_id: '20942'
  file_name: 2025_AstronomyAstrophysics_GrageraMas.pdf
  file_size: 11021467
  relation: main_file
  success: 1
file_date_updated: 2026-01-05T11:06:16Z
has_accepted_license: '1'
intvolume: '       704'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A kinematic history of stellar encounters with Beta Pictoris
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 704
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '20931'
abstract:
- lang: eng
  text: "Context. Asymmetries in the observed rotational splittings of a multiplet
    contain information about the star’s rotation profile and internal magnetic field.
    Moreover, the frequency regularities of multiplets can be used for mode identification.
    However, to exploit this information, highly accurate theoretical predictions
    are needed.\r\n\r\nAims. We aim to quantify the difference in the predicted mode
    asymmetries between a 1D perturbative method and a 2D method that includes a 2D
    stellar structure model, which takes rotation into account. We then place these
    differences between 1D and 2D methods in the context of asteroseismic measurements
    of internal magnetic fields. We only focus on the asymmetries and not on possible
    additional frequency peaks that can arise when the magnetic and rotation axis
    are misaligned.\r\n\r\nMethods. We coupled the 1D pulsation codes GYRE and StORM
    to the 2D stellar structure code ESTER and compared the oscillation predictions
    with the results from the 2D TOP pulsation code. We focused on zero-age main-sequence
    models representative of rotating β Cephei pulsators spinning at up to 20 per
    cent of the critical Keplerian rotation rate. Specifically, we investigated low-radial-order
    gravity and pressure modes.\r\n\r\nResults. We find a generally good agreement
    between the oscillation frequencies resulting from the 1D and 2D pulsation codes.
    We report differences in predicted mode multiplet asymmetries of mostly below
    0.06 d−1. Since the magnetic asymmetries are small compared to the differences
    in the rotational asymmetries resulting from the 1D and 2D predictions, accurate
    measurements of the magnetic field are in most cases challenging.\r\n\r\nConclusions.
    Differences in the predicted mode asymmetries of a rotating star between 1D perturbative
    methods and 2D non-perturbative methods can greatly hinder accurate measurements
    of internal magnetic fields in main-sequence pulsators with low-order modes. Nevertheless,
    reasonably accurate measurements could be possible with npg ≥ 2 modes if the internal
    rotation is roughly below 10 per cent of the Keplerian critical rotation frequency
    for (aligned) magnetic fields of the order of a few hundred kilogauss. While the
    differences between the 1D and 2D frequency predictions are mostly too large for
    internal magnetic field detections, the rotational asymmetries predicted by StORM
    are in general accurate enough for asteroseismic modelling of the stellar rotation
    in main-sequence stars with identified low-order modes."
acknowledgement: 'We thank the anonymous referee for their comments on the manuscript,
  Dario Fritzewski for providing the distribution of fractions of critical rotation
  for the β Cephei sample, and Zhao Guo for the discussions. The research leading
  to these results has received funding from the European Research Council (ERC) under
  the Horizon Europe programme (Synergy Grant agreement N°101071505: 4D-STAR). While
  partially funded by the European Union, views and opinions expressed are however
  those of the authors only and do not necessarily reflect those of the European Union
  or the European Research Council. Neither the European Union nor the granting authority
  can be held responsible for them. V.V. acknowledges support from the Research Foundation
  Flanders (FWO) under grant agreement N°1156923N (PhD Fellowship). S.B.D. acknowledges
  funding from the European Union’s Horizon 2020 research and innovation programme
  under the Marie Skłodowska-Curie grant agreement N°101034413. L.B. gratefully acknowledges
  support from the European Research Council (ERC) under the Horizon Europe programme
  (Calcifer; Starting Grant agreement N°101165631). J.B., M.R., S.M. and J.S.G.M have
  been supported by CNES, focused on the preparation of the PLATO mission. Computations
  with ESTER and TOP have made use of the HPC resources from the CALMIP supercomputing
  centre (Grant 2023-P0107). This research made use of the numpy (Harris et al. 2020)
  and matplotlib (Hunter 2007) Python software packages.'
article_number: A336
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J. S.G.
  full_name: Mombarg, J. S.G.
  last_name: Mombarg
- first_name: V.
  full_name: Vanlaer, V.
  last_name: Vanlaer
- first_name: Srijan B
  full_name: Das, Srijan B
  id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
  last_name: Das
  orcid: 0000-0003-0896-7972
- first_name: M.
  full_name: Rieutord, M.
  last_name: Rieutord
- first_name: C.
  full_name: Aerts, C.
  last_name: Aerts
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: D. R.
  full_name: Reese, D. R.
  last_name: Reese
- first_name: J.
  full_name: Ballot, J.
  last_name: Ballot
citation:
  ama: Mombarg JSG, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient
    for asteroseismic modelling of β Cephei pulsators? Implications for measurements
    of rotation and internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>.
    2025;704. doi:<a href="https://doi.org/10.1051/0004-6361/202557247">10.1051/0004-6361/202557247</a>
  apa: Mombarg, J. S. G., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet,
    L. A., … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic
    modelling of β Cephei pulsators? Implications for measurements of rotation and
    internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a
    href="https://doi.org/10.1051/0004-6361/202557247">https://doi.org/10.1051/0004-6361/202557247</a>
  chicago: Mombarg, J. S.G., V. Vanlaer, Srijan B Das, M. Rieutord, C. Aerts, Lisa
    Annabelle Bugnet, S. Mathis, D. R. Reese, and J. Ballot. “Is a 1D Perturbative
    Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications
    for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202557247">https://doi.org/10.1051/0004-6361/202557247</a>.
  ieee: J. S. G. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for
    asteroseismic modelling of β Cephei pulsators? Implications for measurements of
    rotation and internal magnetic fields,” <i>Astronomy &#38; Astrophysics</i>, vol.
    704. EDP Sciences, 2025.
  ista: Mombarg JSG, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S,
    Reese DR, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic
    modelling of β Cephei pulsators? Implications for measurements of rotation and
    internal magnetic fields. Astronomy &#38; Astrophysics. 704, A336.
  mla: Mombarg, J. S. G., et al. “Is a 1D Perturbative Method Sufficient for Asteroseismic
    Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and
    Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A336,
    EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202557247">10.1051/0004-6361/202557247</a>.
  short: J.S.G. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet,
    S. Mathis, D.R. Reese, J. Ballot, Astronomy &#38; Astrophysics 704 (2025).
date_created: 2026-01-04T23:01:35Z
date_published: 2025-12-19T00:00:00Z
date_updated: 2026-02-16T12:14:36Z
day: '19'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202557247
ec_funded: 1
external_id:
  arxiv:
  - '2511.09617'
file:
- access_level: open_access
  checksum: d838b4783920c43b7cc866e9cf08b383
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  creator: dernst
  date_created: 2026-01-05T08:36:28Z
  date_updated: 2026-01-05T08:36:28Z
  file_id: '20937'
  file_name: 2025_AstronomyAstrophysics_Mombarg.pdf
  file_size: 2620909
  relation: main_file
  success: 1
file_date_updated: 2026-01-05T08:36:28Z
has_accepted_license: '1'
intvolume: '       704'
language:
- iso: eng
month: '12'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
- _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9
  grant_number: '101165631'
  name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology'
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
related_material:
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  - id: '20936'
    relation: research_data
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scopus_import: '1'
status: public
title: Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei
  pulsators? Implications for measurements of rotation and internal magnetic fields
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 704
year: '2025'
...
---
OA_place: repository
OA_type: gold
_id: '20936'
abstract:
- lang: eng
  text: "Supplementary material for Mombarg et al. (2025, A&A). Title: \"Is a 1D perturbative
    method sufficient for asteroseismic modelling of \r\n~Cephei pulsators? Implications
    for measurements of rotation and internal magnetic fields\"\r\n\r\nContent:\r\n-
    Non-rotating ESTER models and associated .GSM models. (Xini = 0.71, Zini = 0.014,
    vertical/horizonal viscosity 10^7 cm^2/s, vertical chemical diffusion 10^4 cm^2/s
    for evolution model. More details on the ESTER models can be found in the ESTER
    manual.\r\n\r\n- Rotational asymmetries computed with StORM and TOP in 1/d, and
    the central m=0 frequency from TOP in 1/d. (all_A*_new.pkl)\r\n\r\n- Magnetic
    asymmetries in 1/d for different obliquity angles between 0 and 90 deg for ZAMS
    and MAMS model, for B_0 = 75 kG. *_nu key gives unperturbed mode frequencies,
    *_npg the radial order (asym_dict.pkl, asym_dict_evol.pkl)"
article_processing_charge: No
author:
- first_name: Joey
  full_name: Mombarg, Joey
  last_name: Mombarg
- first_name: Vincent
  full_name: Vanlaer, Vincent
  last_name: Vanlaer
- first_name: Srijan B
  full_name: Das, Srijan B
  id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
  last_name: Das
  orcid: 0000-0003-0896-7972
- first_name: Michel
  full_name: Rieutord, Michel
  last_name: Rieutord
- first_name: Conny
  full_name: Aerts, Conny
  last_name: Aerts
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: Stephane
  full_name: Mathis, Stephane
  last_name: Mathis
- first_name: Daniel
  full_name: Reese, Daniel
  last_name: Reese
- first_name: Jerome
  full_name: Ballot, Jerome
  last_name: Ballot
citation:
  ama: Mombarg J, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient
    for asteroseismic modelling of β Cephei pulsators? 2025. doi:<a href="https://doi.org/10.5281/ZENODO.17580178">10.5281/ZENODO.17580178</a>
  apa: Mombarg, J., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet, L. A.,
    … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic
    modelling of β Cephei pulsators? Zenodo. <a href="https://doi.org/10.5281/ZENODO.17580178">https://doi.org/10.5281/ZENODO.17580178</a>
  chicago: Mombarg, Joey, Vincent Vanlaer, Srijan B Das, Michel Rieutord, Conny Aerts,
    Lisa Annabelle Bugnet, Stephane Mathis, Daniel Reese, and Jerome Ballot. “Is a
    1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators?”
    Zenodo, 2025. <a href="https://doi.org/10.5281/ZENODO.17580178">https://doi.org/10.5281/ZENODO.17580178</a>.
  ieee: J. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic
    modelling of β Cephei pulsators?” Zenodo, 2025.
  ista: Mombarg J, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S, Reese
    D, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic modelling
    of β Cephei pulsators?, Zenodo, <a href="https://doi.org/10.5281/ZENODO.17580178">10.5281/ZENODO.17580178</a>.
  mla: Mombarg, Joey, et al. <i>Is a 1D Perturbative Method Sufficient for Asteroseismic
    Modelling of β Cephei Pulsators?</i> Zenodo, 2025, doi:<a href="https://doi.org/10.5281/ZENODO.17580178">10.5281/ZENODO.17580178</a>.
  short: J. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S.
    Mathis, D. Reese, J. Ballot, (2025).
date_created: 2026-01-05T08:39:33Z
date_published: 2025-11-11T00:00:00Z
date_updated: 2026-02-16T12:14:36Z
day: '11'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.5281/ZENODO.17580178
main_file_link:
- open_access: '1'
  url: https://doi.org/10.5281/zenodo.17580178
month: '11'
oa: 1
oa_version: Submitted Version
publisher: Zenodo
related_material:
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    relation: used_in_publication
    status: public
status: public
title: Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei
  pulsators?
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: research_data_reference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '21252'
abstract:
- lang: eng
  text: "Context. Recent observational results from asteroseismic studies show that
    an important fraction of solar-like stars do not present detectable stochastically
    excited acoustic oscillations. This non-detectability seems to correlate with
    a high rotation rate in the convective envelope and a high surface magnetic activity.
    At the same time, the properties of stellar convection are affected by rotation
    and magnetism.\r\nAims. We investigate the role of rotation in the excitation
    of acoustic modes in the convective envelope of solar-like stars, to evaluate
    its impact on the energy injected in the oscillations.\r\nMethods. We derived
    theoretical prescriptions for the excitation of acoustic waves in the convective
    envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory
    to model the influence of rotation on convection. We used the MESA stellar evolution
    code and the GYRE stellar oscillation code to estimate the power injected in the
    oscillations from our theoretical prescriptions.\r\nResults. We demonstrate that
    the power injected in the acoustic modes is insensitive to rotation if a Gaussian
    time-correlation function is assumed, while it can decrease by up to 60% for a
    Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that
    the modification of the excitation rate by rotation depends not only on the rotation
    rate but also on the radial and angular orders of the considered oscillation mode.
    This result can allow for better constraints on the properties of stellar convection
    by studying observationally acoustic mode excitation.\r\nConclusions. These results
    demonstrate how important it is to take into account the modification of stellar
    convection by rotation when evaluating the amplitude of the stellar oscillations
    it stochastically excites. They open the path for understanding the large variety
    of observed acoustic-mode amplitudes at the surface of solar-like stars as a function
    of surface rotation rates."
acknowledgement: 'The authors thank the referee for detailed comments that allow them
  to improve their work. The authors thank Jordan Philidet and Kevin Belkacem for
  fruitful discussions. L.B. and Stéphane M. acknowledge support from the European
  Research Council (ERC) under the Horizon Europe program (Synergy Grant agreement
  101071505: 4D-STAR), from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from
  PNPS (CNRS/INSU). While partially funded by the European Union, views and opinions
  expressed are however those of the author only and do not necessarily reflect those
  of the European Union or the European Research Council. Neither the European Union
  nor the granting authority can be held responsible for them. Savita M. acknowledges
  support from the Spanish Ministry of Science and Innovation with the grant no. PID2019-107061GB-C66
  and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023
  (CEX2019-000920-S).'
article_number: A25
article_processing_charge: Yes
article_type: original
author:
- first_name: L.
  full_name: Bessila, L.
  last_name: Bessila
- first_name: A.
  full_name: Deckx van Ruys, A.
  last_name: Deckx van Ruys
- first_name: V.
  full_name: Buriasco, V.
  last_name: Buriasco
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: R. A.
  full_name: García, R. A.
  last_name: García
- first_name: S.
  full_name: Mathur, S.
  last_name: Mathur
citation:
  ama: Bessila L, Deckx van Ruys A, Buriasco V, et al. The impact of rotation on the
    stochastic excitation of stellar acoustic modes in solar-like pulsators. <i>Astronomy
    &#38; Astrophysics</i>. 2025;700. doi:<a href="https://doi.org/10.1051/0004-6361/202452093">10.1051/0004-6361/202452093</a>
  apa: Bessila, L., Deckx van Ruys, A., Buriasco, V., Mathis, S., Bugnet, L. A., García,
    R. A., &#38; Mathur, S. (2025). The impact of rotation on the stochastic excitation
    of stellar acoustic modes in solar-like pulsators. <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202452093">https://doi.org/10.1051/0004-6361/202452093</a>
  chicago: Bessila, L., A. Deckx van Ruys, V. Buriasco, S. Mathis, Lisa Annabelle
    Bugnet, R. A. García, and S. Mathur. “The Impact of Rotation on the Stochastic
    Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2025. <a href="https://doi.org/10.1051/0004-6361/202452093">https://doi.org/10.1051/0004-6361/202452093</a>.
  ieee: L. Bessila <i>et al.</i>, “The impact of rotation on the stochastic excitation
    of stellar acoustic modes in solar-like pulsators,” <i>Astronomy &#38; Astrophysics</i>,
    vol. 700. EDP Sciences, 2025.
  ista: Bessila L, Deckx van Ruys A, Buriasco V, Mathis S, Bugnet LA, García RA, Mathur
    S. 2025. The impact of rotation on the stochastic excitation of stellar acoustic
    modes in solar-like pulsators. Astronomy &#38; Astrophysics. 700, A25.
  mla: Bessila, L., et al. “The Impact of Rotation on the Stochastic Excitation of
    Stellar Acoustic Modes in Solar-like Pulsators.” <i>Astronomy &#38; Astrophysics</i>,
    vol. 700, A25, EDP Sciences, 2025, doi:<a href="https://doi.org/10.1051/0004-6361/202452093">10.1051/0004-6361/202452093</a>.
  short: L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A.
    García, S. Mathur, Astronomy &#38; Astrophysics 700 (2025).
date_created: 2026-02-16T15:46:59Z
date_published: 2025-08-01T00:00:00Z
date_updated: 2026-02-17T13:10:18Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202452093
file:
- access_level: open_access
  checksum: b8a0927307c1d82025bcb5af47b20b26
  content_type: application/pdf
  creator: dernst
  date_created: 2026-02-17T13:07:45Z
  date_updated: 2026-02-17T13:07:45Z
  file_id: '21306'
  file_name: 2025_AstronomyAstrophysics_Bessila.pdf
  file_size: 7161755
  relation: main_file
  success: 1
file_date_updated: 2026-02-17T13:07:45Z
has_accepted_license: '1'
intvolume: '       700'
language:
- iso: eng
month: '08'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
status: public
title: The impact of rotation on the stochastic excitation of stellar acoustic modes
  in solar-like pulsators
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 700
year: '2025'
...
---
OA_place: publisher
OA_type: hybrid
_id: '19637'
abstract:
- lang: eng
  text: PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed
    to detect and characterise extrasolar planets and perform asteroseismic monitoring
    of a large number of stars. PLATO will detect small planets (down to <2R Earth)
    around bright stars (<11 mag), including terrestrial planets in the habitable
    zone of solar-like stars. With the complement of radial velocity observations
    from the ground, planets will be characterised for their radius, mass, and age
    with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO
    will provide us with a large-scale catalogue of well-characterised small planets
    up to intermediate orbital periods, relevant for a meaningful comparison to planet
    formation theories and to better understand planet evolution. It will make possible
    comparative exoplanetology to place our Solar System planets in a broader context.
    In parallel, PLATO will study (host) stars using asteroseismology, allowing us
    to determine the stellar properties with high accuracy, substantially enhancing
    our knowledge of stellar structure and evolution. The payload instrument consists
    of 26 cameras with 12cm aperture each. For at least four years, the mission will
    perform high-precision photometric measurements. Here we review the science objectives,
    present PLATO‘s target samples and fields, provide an overview of expected core
    science performance as well as a description of the instrument and the mission
    profile towards the end of the serial production of the flight cameras. PLATO
    is scheduled for a launch date end 2026. This overview therefore provides a summary
    of the mission to the community in preparation of the upcoming operational phases.
acknowledgement: Open Access funding enabled and organized by Projekt DEAL.
article_number: '26'
article_processing_charge: Yes (via OA deal)
article_type: original
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  full_name: Pollacco, Don
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  full_name: Ragazzoni, Roberto
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  full_name: Christensen-Dalsgaard, Jørgen
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  full_name: Correia, Alexandre C.M.
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  full_name: Gomes Da Silva, João
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  full_name: Gómez Zazo, Luis Jorge
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- first_name: Jonay Isai
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- first_name: Eike Wolf
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- first_name: Terrasa
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- first_name: Janis
  full_name: Hagelberg, Janis
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- first_name: Johann
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  last_name: Hasiba
- first_name: Carole A.
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  last_name: Kennedy
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- first_name: Franz
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  full_name: Kidger, Mark
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- first_name: Flavien
  full_name: Kiefer, Flavien
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- first_name: Christian
  full_name: Kintziger, Christian
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- first_name: Kristina
  full_name: Kislyakova, Kristina
  last_name: Kislyakova
- first_name: László
  full_name: Kiss, László
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  full_name: Klagyivik, Peter
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- first_name: Hubert
  full_name: Klahr, Hubert
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- first_name: Jonas
  full_name: Klevas, Jonas
  last_name: Klevas
- first_name: Oleg
  full_name: Kochukhov, Oleg
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  full_name: Köhler, Ulrich
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  last_name: Kovács
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  full_name: Laky, Gunter
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  full_name: Lam, Kristine Wai Fun
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  full_name: Lambrechts, Michiel
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  full_name: Michaelis, Harald
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  full_name: Michtchenko, Tatiana
  last_name: Michtchenko
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  full_name: Miglio, Andrea
  last_name: Miglio
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  full_name: Miguel, Yamila
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  last_name: Milligan
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  full_name: Mirouh, Giovanni
  last_name: Mirouh
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  full_name: Mitchell, Morgan
  last_name: Mitchell
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  last_name: Moedas
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  full_name: Molnár, László
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  full_name: Mombarg, Joey
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  full_name: Montalto, Marco
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  full_name: Monteiro, Mário J.P.F.G.
  last_name: Monteiro
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  last_name: Montoro Sánchez
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  full_name: Morales, Juan Carlos
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  full_name: Mordasini, Christoph
  last_name: Mordasini
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  full_name: Moreau, Chrystel
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  last_name: Moya
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  full_name: Muehlmann, Prisca
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  full_name: Muirhead, Philip
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  full_name: Musella, Ilaria
  last_name: Musella
- first_name: Alexander James
  full_name: Mustill, Alexander James
  last_name: Mustill
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  full_name: Nardetto, Nicolas
  last_name: Nardetto
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  full_name: Nash, Anna
  last_name: Nash
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  last_name: Neiner
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  full_name: Nelson, Richard P.
  last_name: Nelson
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  full_name: Noels-Grotsch, Arlette
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  full_name: Norazman, Azib
  last_name: Norazman
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  full_name: Norton, Andrew J.
  last_name: Norton
- first_name: Benard
  full_name: Nsamba, Benard
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  last_name: Ofir
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  full_name: Ogilvie, Gordon
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  last_name: Olivetto
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  full_name: Olofsson, Göran
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  full_name: Ong, Joel
  last_name: Ong
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  full_name: Ortolani, Sergio
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  full_name: Oshagh, Mahmoudreza
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  full_name: Ottacher, Harald
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  full_name: Ouazzani, Rhita Maria
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  full_name: Paproth, Carsten
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  full_name: Parviainen, Hannu
  last_name: Parviainen
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  full_name: Pascual Granado, Javier
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  last_name: Pätzold
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  full_name: Pedersen, May Gade
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  full_name: Pena Hidalgo, David
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  full_name: Persson, Carina M.
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  full_name: Pertenais, Martin
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  full_name: Peter, Gisbert
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  full_name: Pietrinferni, Adriano
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  full_name: Plasson, Philippe
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  full_name: Poppenhaeger, Katja
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  full_name: Portaluri, Elisa
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  full_name: Porto De Mello, Gustavo Frederico
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  full_name: Poyatos, Julien
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  full_name: Pozuelos, Francisco J.
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  full_name: Quade, Matthias
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  full_name: Quirrenbach, Andreas
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  full_name: Rabanal Reina, Julio Arturo
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  full_name: Raimondo, Gabriella
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  full_name: Rainer, Monica
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  full_name: Ramón Rodón, Jose
  last_name: Ramón Rodón
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  full_name: Ramón-Ballesta, Alejandro
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  full_name: Ramos Zapata, Gonzalo
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  last_name: Redmer
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  full_name: Ribas, Ignasi
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  full_name: Rice, Ken
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  full_name: Riello, Marco
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  full_name: Rieutord, Michel
  last_name: Rieutord
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  full_name: Ripepi, Vincenzo
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  full_name: Rockstein, Steve
  last_name: Rockstein
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  full_name: Rodríguez Amor, Alberto
  last_name: Rodríguez Amor
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  full_name: Rodriguez Garcia, Juan Pablo
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  full_name: Rodriguez-Gomez, Julio
  last_name: Rodriguez-Gomez
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  full_name: Roehlly, Yannick
  last_name: Roehlly
- first_name: Fernando
  full_name: Roig, Fernando
  last_name: Roig
- first_name: Bárbara
  full_name: Rojas-Ayala, Bárbara
  last_name: Rojas-Ayala
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  full_name: Rolf, Tobias
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- first_name: Jakob Lysgaard
  full_name: Rørsted, Jakob Lysgaard
  last_name: Rørsted
- first_name: Hugo
  full_name: Rosado, Hugo
  last_name: Rosado
- first_name: Giovanni
  full_name: Rosotti, Giovanni
  last_name: Rosotti
- first_name: Olivier
  full_name: Roth, Olivier
  last_name: Roth
- first_name: Markus
  full_name: Roth, Markus
  last_name: Roth
- first_name: Alex
  full_name: Rousseau, Alex
  last_name: Rousseau
- first_name: Ian
  full_name: Roxburgh, Ian
  last_name: Roxburgh
- first_name: Fabrice
  full_name: Roy, Fabrice
  last_name: Roy
- first_name: Pierre
  full_name: Royer, Pierre
  last_name: Royer
- first_name: Kirk
  full_name: Ruane, Kirk
  last_name: Ruane
- first_name: Sergio
  full_name: Rufini Mastropasqua, Sergio
  last_name: Rufini Mastropasqua
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- first_name: Martin
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- first_name: Edward
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- first_name: Jesper
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- first_name: Russel
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- first_name: Axelle
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- first_name: Kyle
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  last_name: Silliman
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  full_name: Silvotti, Roberto
  last_name: Silvotti
- first_name: Attila E.
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- first_name: Marek
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  last_name: Skarka
- first_name: Barry
  full_name: Smalley, Barry
  last_name: Smalley
- first_name: Rodolfo
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- first_name: Samuel
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- first_name: Alexis
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  last_name: Smith
- first_name: Leigh
  full_name: Smith, Leigh
  last_name: Smith
- first_name: Ignas
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- first_name: Ádám
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- first_name: Frank
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- first_name: Francesca
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  last_name: Sortino
- first_name: Sérgio
  full_name: Sousa, Sérgio
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- first_name: John
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  last_name: Southworth
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  full_name: Souto, Diogo
  last_name: Souto
- first_name: Alessandro
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- first_name: Dimitris
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- first_name: Keivan
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  last_name: Stassun
- first_name: Manfred
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  full_name: Stello, Dennis
  last_name: Stello
- first_name: Beate
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  last_name: Stiebeler
- first_name: Amalie
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  last_name: Stokholm
- first_name: Trude
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- first_name: Klaus
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- first_name: Paul Anthony
  full_name: Strøm, Paul Anthony
  last_name: Strøm
- first_name: Antoine
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  last_name: Strugarek
- first_name: Sophia
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  last_name: Sulis
- first_name: Michal
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- first_name: László
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- first_name: Geert Jan
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- first_name: Daniele
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- first_name: Tom
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- first_name: Frédéric
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- first_name: Anne
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- first_name: Didier
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- first_name: Ruth
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- first_name: Andrew
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- first_name: Daniel
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- first_name: Nicola
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- first_name: Regner
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- first_name: Reidar
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- first_name: Matthias
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- first_name: Konstantinos
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- first_name: Antonio
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- first_name: Sergey
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    D. Huber, J. Huesler, A. Hui-Bon-Hoa, R. Huygen, D.D. Huynh, N. Iro, J. Irwin,
    M. Irwin, A. Izidoro, S. Jacquinod, N.E. Jannsen, M. Janson, H. Jeszenszky, C.
    Jiang, A.J. Jimenez Mancebo, P. Jofre, A. Johansen, C. Johnston, G. Jones, T.
    Kallinger, S. Kálmán, T. Kanitz, M. Karjalainen, R. Karjalainen, C. Karoff, S.
    Kawaler, D. Kawata, A. Keereman, D. Keiderling, T. Kennedy, M. Kenworthy, F. Kerschbaum,
    M. Kidger, F. Kiefer, C. Kintziger, K. Kislyakova, L. Kiss, P. Klagyivik, H. Klahr,
    J. Klevas, O. Kochukhov, U. Köhler, U. Kolb, A. Koncz, J. Korth, N. Kostogryz,
    G. Kovács, J. Kovács, O. Kozhura, N. Krivova, A. Kuĉinskas, I. Kuhlemann, F. Kupka,
    W. Laauwen, A. Labiano, N. Lagarde, P. Laget, G. Laky, K.W.F. Lam, M. Lambrechts,
    H. Lammer, A.F. Lanza, A. Lanzafame, M. Lares Martiz, J. Laskar, H. Latter, T.
    Lavanant, A. Lawrenson, C. Lazzoni, A. Lebre, Y. Lebreton, A. Lecavelier Des Etangs,
    K. Lee, Z. Leinhardt, A. Leleu, M. Lendl, G. Leto, Y. Levillain, A.S. Libert,
    T. Lichtenberg, R. Ligi, F. Lignieres, J. Lillo-Box, J. Linsky, J.S. Liu, D. Loidolt,
    Y. Longval, I. Lopes, A. Lorenzani, H.G. Ludwig, M. Lund, M.S. Lundkvist, X. Luri,
    C. Maceroni, S. Madden, N. Madhusudhan, A. Maggio, C. Magliano, D. Magrin, L.
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    H. Michaelis, E. Michel, M. Michielsen, T. Michtchenko, A. Miglio, Y. Miguel,
    D. Milligan, G. Mirouh, M. Mitchell, N. Moedas, F. Molendini, L. Molnár, J. Mombarg,
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    J. Ong, S. Ortolani, M. Oshagh, H. Ottacher, R. Ottensamer, R.M. Ouazzani, S.J.
    Paardekooper, E. Pace, M. Pajas, A. Palacios, G. Palandri, E. Palle, C. Paproth,
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    M. Pertenais, G. Peter, A.C. Petit, P. Petit, S. Pezzuto, G. Pichierri, A. Pietrinferni,
    F. Pinheiro, M. Pinsonneault, E. Plachy, P. Plasson, B. Plez, K. Poppenhaeger,
    E. Poretti, E. Portaluri, J. Portell, G.F. Porto De Mello, J. Poyatos, F.J. Pozuelos,
    P.G. Prada Moroni, D. Pricopi, L. Prisinzano, M. Quade, A. Quirrenbach, J.A. Rabanal
    Reina, M.C. Rabello Soares, G. Raimondo, M. Rainer, J. Ramón Rodón, A. Ramón-Ballesta,
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    Ortiz, M.T. Rodrigo Rodríguez, A. Rodríguez Amor, L.F. Rodríguez Díaz, J.P. Rodriguez
    Garcia, J. Rodriguez-Gomez, Y. Roehlly, F. Roig, B. Rojas-Ayala, T. Rolf, J.L.
    Rørsted, H. Rosado, G. Rosotti, O. Roth, M. Roth, A. Rousseau, I. Roxburgh, F.
    Roy, P. Royer, K. Ruane, S. Rufini Mastropasqua, C. Ruiz De Galarreta, A. Russi,
    S. Saar, M. Saillenfest, M. Salaris, S. Salmon, I. Saltas, R. Samadi, A. Samadi,
    D. Samra, T. Sanches Da Silva, M.A. Sánchez Carrasco, A. Santerne, A. Santiago
    Pé, F. Santoli, Ä.R.G. Santos, R. Sanz Mesa, L.M. Sarro, G. Scandariato, M. Schäfer,
    E. Schlafly, F.X. Schmider, J. Schneider, J. Schou, H. Schunker, G.J. Schwarzkopf,
    A. Serenelli, D. Seynaeve, Y. Shan, A. Shapiro, R. Shipman, D. Sicilia, M.A. Sierra
    Sanmartin, A. Sigot, K. Silliman, R. Silvotti, A.E. Simon, R. Simoyama Napoli,
    M. Skarka, B. Smalley, R. Smiljanic, S. Smit, A. Smith, L. Smith, I. Snellen,
    Á. Sódor, F. Sohl, S.K. Solanki, F. Sortino, S. Sousa, J. Southworth, D. Souto,
    A. Sozzetti, D. Stamatellos, K. Stassun, M. Steller, D. Stello, B. Stelzer, U.
    Stiebeler, A. Stokholm, T. Storelvmo, K. Strassmeier, P.A. Strøm, A. Strugarek,
    S. Sulis, M. Švanda, L. Szabados, R. Szabó, G.M. Szabó, E. Szuszkiewicz, G.J.
    Talens, D. Teti, T. Theisen, F. Thévenin, A. Thoul, D. Tiphene, R. Titz-Weider,
    A. Tkachenko, D. Tomecki, J. Tonfat, N. Tosi, R. Trampedach, G. Traven, A. Triaud,
    R. Trønnes, M. Tsantaki, M. Tschentscher, A. Turin, A. Tvaruzka, B. Ulmer, S.
    Ulmer-Moll, C. Ulusoy, G. Umbriaco, D. Valencia, M. Valentini, A. Valio, Á.L.
    Valverde Guijarro, V. Van Eylen, V. Van Grootel, T.A. Van Kempen, T. Van Reeth,
    I. Van Zelst, B. Vandenbussche, K. Vasiliou, V. Vasilyev, D. Vaz De Mascarenhas,
    A. Vazan, M. Vela Nunez, E.N. Velloso, R. Ventura, P. Ventura, J. Venturini, I.
    Vera Trallero, D. Veras, E. Verdugo, K. Verma, D. Vibert, T. Vicanek Martinez,
    K. Vida, A. Vigan, A. Villacorta, E. Villaver, M. Villaverde Aparicio, V. Viotto,
    E. Vorobyov, S. Vorontsov, F.W. Wagner, N. Walton, D. Walton, H. Wang, R. Waters,
    C. Watson, S. Wedemeyer, A. Weeks, J. Weingrill, A. Weiss, B. Wendler, R. West,
    K. Westerdorff, P.A. Westphal, P. Wheatley, T. White, A. Whittaker, K. Wickhusen,
    T. Wilson, J. Windsor, O. Winter, M.L. Winther, A. Winton, U. Witteck, V. Witzke,
    P. Woitke, D. Wolter, G. Wuchterl, M. Wyatt, D. Yang, J. Yu, R. Zanmar Sanchez,
    M.R. Zapatero Osorio, M. Zechmeister, Y. Zhou, C. Ziemke, K. Zwintz, T. Böhm,
    L.M. Dansac, Experimental Astronomy 59 (2025).
date_created: 2025-05-04T22:02:30Z
date_published: 2025-04-21T00:00:00Z
date_updated: 2026-04-02T11:44:00Z
day: '21'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1007/s10686-025-09985-9
external_id:
  isi:
  - '001498306700001'
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oa_version: Published Version
publication: Experimental Astronomy
publication_identifier:
  eissn:
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  issn:
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publication_status: published
publisher: Springer Nature
quality_controlled: '1'
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status: public
title: The PLATO mission
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 59
year: '2025'
...
---
OA_place: repository
OA_type: green
_id: '21309'
abstract:
- lang: eng
  text: The polarization of light is a critically under-utilized, rich source of information
    in astronomy. For stars in particular, surface magnetism polarization that can
    be detected and measured with spectro-polarimetry. Many questions about these
    surface fields remain unanswered due to a lack of dedicated instruments capable
    of probing weak and strong surface magnetic fields for the entire mass range of
    stars, from M-dwarfs (and even substellar objects) to massive O-type stars at
    different evolutionary stages and metallicities. These questions range from the
    origin of these fields to their true incidence rate throughout the stellar population
    and the dependence on metallicity. Magnetic fields, although currently often excluded
    from stellar evolution models, play an important role in stellar evolution. Connecting
    the surface fields to internal fields through asteroseismology will instigate
    a new era of understanding stellar evolution and the transport of angular momentum
    and chemical elements throughout stellar interiors, also impacting our understanding
    of star-planet interactions and stellar remnants. Polarimetry is also an under-utilized
    tool to observationally constrain the mode identification of nonradial oscillations,
    which lies at the basis of accurate asteroseismic parameter estimation at percentage-level
    for stellar radii, masses, ages, internal rotation, and magnetic field strengths.
    Combining strong constraints on mode identification and surface magnetic properties
    through the acquisition of time-resolved, high-resolution and high-signal-to-noise
    (S/N) spectro-polarimetry and spectroscopy promises to bring leaps forward in
    our understanding of stellar structure, particularly when combined with long-term
    space photometric data from past, current, and future missions.
article_number: '2512.15170'
article_processing_charge: No
arxiv: 1
author:
- first_name: J.
  full_name: Vandersnickt, J.
  last_name: Vandersnickt
- first_name: R. Ochoa
  full_name: Armenta, R. Ochoa
  last_name: Armenta
- first_name: V.
  full_name: Vanlaer, V.
  last_name: Vanlaer
- first_name: A. David-Uraz
  full_name: A. David-Uraz, A. David-Uraz
  last_name: A. David-Uraz
- first_name: C.
  full_name: Aerts, C.
  last_name: Aerts
- first_name: S. B.
  full_name: Das, S. B.
  last_name: Das
- first_name: J. -C.
  full_name: Bouret, J. -C.
  last_name: Bouret
- first_name: D. M.
  full_name: Bowman, D. M.
  last_name: Bowman
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: V.
  full_name: Khalack, V.
  last_name: Khalack
- first_name: J. Labadie-Bartz
  full_name: J. Labadie-Bartz, J. Labadie-Bartz
  last_name: J. Labadie-Bartz
- first_name: S.
  full_name: Mathis, S.
  last_name: Mathis
- first_name: Y.
  full_name: Nazé, Y.
  last_name: Nazé
- first_name: C.
  full_name: Neiner, C.
  last_name: Neiner
- first_name: P.
  full_name: Petit, P.
  last_name: Petit
- first_name: V.
  full_name: Petit, V.
  last_name: Petit
- first_name: K. Thomson-Paressant
  full_name: K. Thomson-Paressant, K. Thomson-Paressant
  last_name: K. Thomson-Paressant
- first_name: T. Van
  full_name: Doorsselaere, T. Van
  last_name: Doorsselaere
- first_name: M.
  full_name: Vanrespaille, M.
  last_name: Vanrespaille
citation:
  ama: Vandersnickt J, Armenta RO, Vanlaer V, et al. Expanding stellar horizons with
    polarized light. <i>arXiv</i>. doi:<a href="https://doi.org/10.48550/arXiv.2512.15170">10.48550/arXiv.2512.15170</a>
  apa: Vandersnickt, J., Armenta, R. O., Vanlaer, V., A. David-Uraz, A. D.-U., Aerts,
    C., Das, S. B., … Vanrespaille, M. (n.d.). Expanding stellar horizons with polarized
    light. <i>arXiv</i>. <a href="https://doi.org/10.48550/arXiv.2512.15170">https://doi.org/10.48550/arXiv.2512.15170</a>
  chicago: Vandersnickt, J., R. Ochoa Armenta, V. Vanlaer, A. David-Uraz A. David-Uraz,
    C. Aerts, S. B. Das, J. -C. Bouret, et al. “Expanding Stellar Horizons with Polarized
    Light.” <i>ArXiv</i>, n.d. <a href="https://doi.org/10.48550/arXiv.2512.15170">https://doi.org/10.48550/arXiv.2512.15170</a>.
  ieee: J. Vandersnickt <i>et al.</i>, “Expanding stellar horizons with polarized
    light,” <i>arXiv</i>. .
  ista: Vandersnickt J, Armenta RO, Vanlaer V, A. David-Uraz AD-U, Aerts C, Das SB,
    Bouret J-C, Bowman DM, Bugnet LA, Khalack V, J. Labadie-Bartz JL-B, Mathis S,
    Nazé Y, Neiner C, Petit P, Petit V, K. Thomson-Paressant KT-P, Doorsselaere TV,
    Vanrespaille M. Expanding stellar horizons with polarized light. arXiv, 2512.15170.
  mla: Vandersnickt, J., et al. “Expanding Stellar Horizons with Polarized Light.”
    <i>ArXiv</i>, 2512.15170, doi:<a href="https://doi.org/10.48550/arXiv.2512.15170">10.48550/arXiv.2512.15170</a>.
  short: J. Vandersnickt, R.O. Armenta, V. Vanlaer, A.D.-U. A. David-Uraz, C. Aerts,
    S.B. Das, J.-C. Bouret, D.M. Bowman, L.A. Bugnet, V. Khalack, J.L.-B. J. Labadie-Bartz,
    S. Mathis, Y. Nazé, C. Neiner, P. Petit, V. Petit, K.T.-P. K. Thomson-Paressant,
    T.V. Doorsselaere, M. Vanrespaille, ArXiv (n.d.).
date_created: 2026-02-17T13:53:50Z
date_published: 2025-12-17T00:00:00Z
date_updated: 2026-04-07T06:00:40Z
day: '17'
department:
- _id: LiBu
doi: 10.48550/arXiv.2512.15170
external_id:
  arxiv:
  - '2512.15170'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.2512.15170
month: '12'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
status: public
title: Expanding stellar horizons with polarized light
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2025'
...
---
OA_place: publisher
_id: '19853'
abstract:
- lang: eng
  text: "The internal dynamical properties of red giant stars have been explored extensively
    in recent\r\nyears as a result of the increase in high precision data availability
    from the space missions\r\nKepler and TESS (Transiting Exoplanet Survey Satellite),
    and in this exploration, it has been\r\ndiscovered that some of these stars are
    not behaving as expected. Red giants are stars that have\r\nevolved off of the
    main sequence after having completed fusing hydrogen into helium in their\r\ncore.
    Observational data shows that the cores are rotating significantly slower than
    models can\r\nrecreate consistently across evolutionary stages. This discrepancy
    has prompted investigation\r\ninto the efficiency of angular momentum transport
    mechanisms and mixing processes including\r\nmeridional circulation, shear instability,
    internal gravity waves, Tayler-Spruit dynamo, fossil\r\nmagnetic fields etc.,
    to explain this behavior.\r\nAnalyzing seismic oscillations in stars, via asteroseismology,
    is a powerful tool as it is the only\r\nway in which the deep stellar interior
    can be probed and subsequently characterized; this is\r\npossible as global oscillations
    modulating the stellar surface are effected by internal processes.\r\nFor red
    giants, p-modes (pressure modes; resonating through the entire star) and g-modes\r\n(gravity-modes;
    resonating in the radiative interior) couple to create mixed modes. These\r\nmixed
    modes give access to the otherwise hidden stellar interior as g-modes couple to
    p-modes,\r\ndelivering information from the interior to the surface.\r\nInternal
    magnetic signatures have been observationally confirmed in red giant stars via\r\nasteroseismology
    and characterized in two ways. One being that dipole mixed modes with\r\nℓ = 1
    will display a global asymmetric frequency shift of its azimuthal components;
    where\r\nthe m = 0 and m = ±1 components of the ℓ = 1 dipole mode will be shifted
    by two\r\ndifferent power laws, respectively. And the other being a reduced visibility
    of dipole mixed\r\nmode amplitudes in the power spectra, where stars presenting
    with this feature are denoted as\r\nsuppressed.\r\nSeveral studies of the suppressed
    dipole mixed mode amplitudes have been carried out, but thus\r\nfar, no dedicated
    studies of the asymmetric frequency shifts of suppressed red giants have been\r\nconducted;
    one reason being that the asymmetric frequency shifts cannot be characterized\r\nwhen
    the dipole mixed mode amplitudes are severely reduced in many of the suppressed
    stars.\r\nSincefullysuppressedstarsdonothavedetectablemixed-modestoevaluate, partiallysuppressed\r\nstars,
    that is, red giant stars presenting with suppressed dipole mixed modes in select
    parts of\r\ntheir power spectra rather than across the entire spectra, will be
    the subject of this study as\r\nthe respective mode amplitudes are still visible
    at high frequencies.\r\nAs such, this study will search for asymmetric frequency
    shifts on the dipole mixed\r\nmodes of partially suppressed red giant stars; the
    aim here is to investigate if both\r\nmode suppression and magnetic shifting of
    dipole mixed modes occur simultaneously.\r\nThisstudywillbeconductedbycreatingapipelinetoestimatepriorsofasteroseismicparameters,\r\nuse
    the priors to model the power spectra with the stellar modeling code sloscillations_ISTA,\r\nand
    perform a Bayesian fit of the parameters with the simulated data on the star KIC
    6975038,\r\na target with partially suppressed dipolar mode amplitudes identified
    in the literature, to fit its\r\nmagnetic parameters. I present a novel method
    to model the stellar power spectra of\r\npartially suppressed red giants by application
    of a sigmoid profile to the ℓ= 1 dipolar\r\nmode component of the spectra. With
    the results of this study I aim at constraining\r\nthe cause of this partial dipole
    mode amplitude suppression, allowing for more detailed\r\nstudies regarding their
    astrophysical nature. Furthermore, the long term hope for the method\r\nused in
    this study will be to expand the sample of partially suppressed red giants and
    fit their\r\nasteroseismic parameters accordingly."
acknowledgement: "I would like to give thanks to myself for my hard work on this document.
  This paper includes data collected by the Kepler mission and obtained from the MAST
  data\r\narchive at the Space Telescope Science Institute (STScI). Funding for the
  Kepler mission is\r\nprovided by the NASA Science Mission Directorate. STScI is
  operated by the Association of\r\nUniversities for Research in Astronomy, Inc.,
  under NASA contract NAS 5–26555.\r\n"
alternative_title:
- ISTA Master's Thesis
article_processing_charge: No
author:
- first_name: Kanah
  full_name: Smith, Kanah
  id: 7703505d-3211-11ee-a6a9-a2ab9d936c15
  last_name: Smith
citation:
  ama: Smith K. Exploring internal magnetism in partially suppressed red giant stars.
    2025. doi:<a href="https://doi.org/10.15479/AT-ISTA-19853">10.15479/AT-ISTA-19853</a>
  apa: Smith, K. (2025). <i>Exploring internal magnetism in partially suppressed red
    giant stars</i>. Institute of Science and Technology Austria. <a href="https://doi.org/10.15479/AT-ISTA-19853">https://doi.org/10.15479/AT-ISTA-19853</a>
  chicago: Smith, Kanah. “Exploring Internal Magnetism in Partially Suppressed Red
    Giant Stars.” Institute of Science and Technology Austria, 2025. <a href="https://doi.org/10.15479/AT-ISTA-19853">https://doi.org/10.15479/AT-ISTA-19853</a>.
  ieee: K. Smith, “Exploring internal magnetism in partially suppressed red giant
    stars,” Institute of Science and Technology Austria, 2025.
  ista: Smith K. 2025. Exploring internal magnetism in partially suppressed red giant
    stars. Institute of Science and Technology Austria.
  mla: Smith, Kanah. <i>Exploring Internal Magnetism in Partially Suppressed Red Giant
    Stars</i>. Institute of Science and Technology Austria, 2025, doi:<a href="https://doi.org/10.15479/AT-ISTA-19853">10.15479/AT-ISTA-19853</a>.
  short: K. Smith, Exploring Internal Magnetism in Partially Suppressed Red Giant
    Stars, Institute of Science and Technology Austria, 2025.
corr_author: '1'
date_created: 2025-06-20T13:27:08Z
date_published: 2025-10-08T00:00:00Z
date_updated: 2026-04-07T12:01:37Z
day: '08'
ddc:
- '520'
degree_awarded: MS
department:
- _id: GradSch
- _id: LiBu
doi: 10.15479/AT-ISTA-19853
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has_accepted_license: '1'
keyword:
- asteroseismology
- stellar physics
- red giant
- magnetism
- suppressed
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
page: '38'
publication_identifier:
  issn:
  - 2791-4585
publication_status: published
publisher: Institute of Science and Technology Austria
status: public
supervisor:
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
title: Exploring internal magnetism in partially suppressed red giant stars
type: dissertation
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '18172'
abstract:
- lang: eng
  text: Red Giant stars host solar-like oscillations which have mixed character, being
    sensitive to conditions both in the outer convection zone and deep within the
    interior. The properties of these modes are sensitive to both core rotation and
    magnetic fields. While asteroseismic studies of the former have been done on a
    large scale, studies of the latter are currently limited to tens of stars. We
    aim to produce the first large catalogue of both magnetic and rotational perturbations.
    We jointly constrain these parameters by devising an automated method for fitting
    the power spectra directly. We successfully apply the method to 302 low-luminosity
    red giants. We find a clear bimodality in core rotation rate. The primary peak
    is at δνrot = 0.32 μHz, and the secondary at δνrot = 0.47 μHz. Combining our results
    with literature values, we find that the percentage of stars rotating much more
    rapidly than the population average increases with evolutionary state. We measure
    magnetic splittings of 2σ significance in 23 stars. While the most extreme magnetic
    splitting values appear in stars with masses > 1.1M⊙, implying they formerly hosted
    a convective core, a small but statistically significant magnetic splitting is
    measured at lower masses. Asymmetry between the frequencies of a rotationally
    split multiplet has previously been used to diagnose the presence of a magnetic
    perturbation. We find that of the stars with a significant detection of magnetic
    perturbation, 43\% do not show strong asymmetry. We find no strong evidence of
    correlation between the rotation and magnetic parameters.
acknowledgement: EJH, WJC, and GRD acknowledge the support of Science and Technology
  Facilities Council. MBN acknowledges support from the UK Space Agency. JMJO acknowledges
  support from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001, awarded
  by STScI (Space Telescope Science Institute), which is operated by the Association
  of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
  The authors acknowledge use of the Blue-BEAR HPC service at the University of Birmingham.
  This paper includes data collected by the Kepler mission and obtained from the MAST
  data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler
  mission was provided by the NASA Science Mission Directorate. This work has made
  use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/web/gaia),
  processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).
  Funding for the DPAC was provided by national institutions, in particular the institutions
  participating in the Gaia Multilateral Agreement. This paper received funding from
  the European Research Council (ERC) under the European Union’s Horizon 2020 research
  and innovation programme (CartographY GA. 804752). SD and JB acknowledge support
  from the Centre National d’Etudes Spatiales (CNES).
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Emily J.
  full_name: Hatt, Emily J.
  last_name: Hatt
- first_name: J. M.Joel
  full_name: Ong, J. M.Joel
  last_name: Ong
- first_name: Martin B.
  full_name: Nielsen, Martin B.
  last_name: Nielsen
- first_name: William J.
  full_name: Chaplin, William J.
  last_name: Chaplin
- first_name: Guy R.
  full_name: Davies, Guy R.
  last_name: Davies
- first_name: Sébastien
  full_name: Deheuvels, Sébastien
  last_name: Deheuvels
- first_name: Jérôme
  full_name: Ballot, Jérôme
  last_name: Ballot
- first_name: Gang
  full_name: Li, Gang
  last_name: Li
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
citation:
  ama: Hatt EJ, Ong JMJ, Nielsen MB, et al. Asteroseismic signatures of core magnetism
    and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the
    Royal Astronomical Society</i>. 2024;534(2):1060-1076. doi:<a href="https://doi.org/10.1093/mnras/stae2053">10.1093/mnras/stae2053</a>
  apa: Hatt, E. J., Ong, J. M. J., Nielsen, M. B., Chaplin, W. J., Davies, G. R.,
    Deheuvels, S., … Bugnet, L. A. (2024). Asteroseismic signatures of core magnetism
    and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the
    Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stae2053">https://doi.org/10.1093/mnras/stae2053</a>
  chicago: Hatt, Emily J., J. M.Joel Ong, Martin B. Nielsen, William J. Chaplin, Guy
    R. Davies, Sébastien Deheuvels, Jérôme Ballot, Gang Li, and Lisa Annabelle Bugnet.
    “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity
    Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2024. <a href="https://doi.org/10.1093/mnras/stae2053">https://doi.org/10.1093/mnras/stae2053</a>.
  ieee: E. J. Hatt <i>et al.</i>, “Asteroseismic signatures of core magnetism and
    rotation in hundreds of low-luminosity red giants,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 534, no. 2. Oxford University Press, pp.
    1060–1076, 2024.
  ista: Hatt EJ, Ong JMJ, Nielsen MB, Chaplin WJ, Davies GR, Deheuvels S, Ballot J,
    Li G, Bugnet LA. 2024. Asteroseismic signatures of core magnetism and rotation
    in hundreds of low-luminosity red giants. Monthly Notices of the Royal Astronomical
    Society. 534(2), 1060–1076.
  mla: Hatt, Emily J., et al. “Asteroseismic Signatures of Core Magnetism and Rotation
    in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 534, no. 2, Oxford University Press, 2024, pp. 1060–76, doi:<a
    href="https://doi.org/10.1093/mnras/stae2053">10.1093/mnras/stae2053</a>.
  short: E.J. Hatt, J.M.J. Ong, M.B. Nielsen, W.J. Chaplin, G.R. Davies, S. Deheuvels,
    J. Ballot, G. Li, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society
    534 (2024) 1060–1076.
date_created: 2024-10-06T22:01:11Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T09:53:01Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1093/mnras/stae2053
external_id:
  arxiv:
  - '2409.01157'
  isi:
  - '001320536900011'
file:
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intvolume: '       534'
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month: '10'
oa: 1
oa_version: Published Version
page: 1060-1076
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity
  red giants
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 534
year: '2024'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '18306'
abstract:
- lang: eng
  text: Neutral sodium (Na i) is an alkali metal with a favorable absorption cross
    section such that tenuous gases are easily illuminated at select transiting exoplanet
    systems. We examine both the time-averaged and time-series alkali spectral flux
    individually, over 4 nights at a hot Saturn system on a ∼2.8 day orbit about a
    Sun-like star WASP-49 A. Very Large Telescope/ESPRESSO observations are analyzed,
    providing new constraints. We recover the previously confirmed residual sodium
    flux uniquely when averaged, whereas night-to-night Na i varies by more than an
    order of magnitude. On HARPS/3.6 m Epoch II, we report a Doppler redshift at vΓ,NaD
    = + 9.7 ± 1.6 km s−1 with respect to the planet's rest frame. Upon examining the
    lightcurves, we confirm night-to-night variability, on the order of ∼1%–4% in
    NaD, rarely coinciding with exoplanet transit, not readily explained by stellar
    activity, starspots, tellurics, or the interstellar medium. Coincident with the
    ∼+10 km s−1 Doppler redshift, we detect a transient sodium absorption event dFNaD/F⋆
    = 3.6% ± 1% at a relative difference of ΔFNaD(t) ∼ 4.4% ± 1%, lasting ΔtNaD ≳
    40 minutes. Since exoplanetary alkali signatures are blueshifted due to the natural
    vector of radiation pressure, estimated here at roughly ∼−5.7 km s−1, the radial
    velocity is rather at +15.4 km s−1, far larger than any known exoplanet system.
    Given that the redshift magnitude vΓ is in between the Roche limit and dynamically
    stable satellite orbits, the transient sodium may be a putative indication of
    a natural satellite orbiting WASP-49 A b.
acknowledgement: The research described in this Letter was carried out in part at
  the Jet Propulsion Laboratory, California Institute of Technology, under a contract
  with the National Aeronautics Space Administration, © 2024. California Institute
  of Technology. Government sponsorship acknowledged. A.V.O. and J.V.S. thank M. Lendl
  for constraints and discussions on the mass of WASP-49 A b. S.G.S acknowledges the
  support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE
  (EC).
article_number: L53
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Apurva V.
  full_name: Oza, Apurva V.
  last_name: Oza
- first_name: Julia V.
  full_name: Seidel, Julia V.
  last_name: Seidel
- first_name: H. Jens
  full_name: Hoeijmakers, H. Jens
  last_name: Hoeijmakers
- first_name: Athira
  full_name: Unni, Athira
  last_name: Unni
- first_name: Aurora Y.
  full_name: Kesseli, Aurora Y.
  last_name: Kesseli
- first_name: Carl A.
  full_name: Schmidt, Carl A.
  last_name: Schmidt
- first_name: Thirupathi
  full_name: Sivarani, Thirupathi
  last_name: Sivarani
- first_name: Aaron
  full_name: Bello-Arufe, Aaron
  last_name: Bello-Arufe
- first_name: Andrea
  full_name: Gebek, Andrea
  last_name: Gebek
- first_name: Moritz
  full_name: Meyer Zu Westram, Moritz
  last_name: Meyer Zu Westram
- first_name: Sérgio G.
  full_name: Sousa, Sérgio G.
  last_name: Sousa
- first_name: Rosaly M.C.
  full_name: Lopes, Rosaly M.C.
  last_name: Lopes
- first_name: Renyu
  full_name: Hu, Renyu
  last_name: Hu
- first_name: Katherine
  full_name: De Kleer, Katherine
  last_name: De Kleer
- first_name: Chloe
  full_name: Fisher, Chloe
  last_name: Fisher
- first_name: Sébastien
  full_name: Charnoz, Sébastien
  last_name: Charnoz
- first_name: Ashley D.
  full_name: Baker, Ashley D.
  last_name: Baker
- first_name: Samuel P.
  full_name: Halverson, Samuel P.
  last_name: Halverson
- first_name: Nick M.
  full_name: Schneider, Nick M.
  last_name: Schneider
- first_name: Angelica
  full_name: Psaridi, Angelica
  last_name: Psaridi
- first_name: Aurélien
  full_name: Wyttenbach, Aurélien
  last_name: Wyttenbach
- first_name: Santiago
  full_name: Torres Rodriguez, Santiago
  id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
  last_name: Torres Rodriguez
  orcid: 0000-0002-3150-8988
- first_name: Ishita
  full_name: Bhatnagar, Ishita
  last_name: Bhatnagar
- first_name: Robert E.
  full_name: Johnson, Robert E.
  last_name: Johnson
citation:
  ama: Oza AV, Seidel JV, Hoeijmakers HJ, et al. Redshifted sodium transient near
    exoplanet transit. <i>Astrophysical Journal Letters</i>. 2024;973(2). doi:<a href="https://doi.org/10.3847/2041-8213/ad6b29">10.3847/2041-8213/ad6b29</a>
  apa: Oza, A. V., Seidel, J. V., Hoeijmakers, H. J., Unni, A., Kesseli, A. Y., Schmidt,
    C. A., … Johnson, R. E. (2024). Redshifted sodium transient near exoplanet transit.
    <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href="https://doi.org/10.3847/2041-8213/ad6b29">https://doi.org/10.3847/2041-8213/ad6b29</a>
  chicago: Oza, Apurva V., Julia V. Seidel, H. Jens Hoeijmakers, Athira Unni, Aurora
    Y. Kesseli, Carl A. Schmidt, Thirupathi Sivarani, et al. “Redshifted Sodium Transient
    near Exoplanet Transit.” <i>Astrophysical Journal Letters</i>. IOP Publishing,
    2024. <a href="https://doi.org/10.3847/2041-8213/ad6b29">https://doi.org/10.3847/2041-8213/ad6b29</a>.
  ieee: A. V. Oza <i>et al.</i>, “Redshifted sodium transient near exoplanet transit,”
    <i>Astrophysical Journal Letters</i>, vol. 973, no. 2. IOP Publishing, 2024.
  ista: Oza AV, Seidel JV, Hoeijmakers HJ, Unni A, Kesseli AY, Schmidt CA, Sivarani
    T, Bello-Arufe A, Gebek A, Meyer Zu Westram M, Sousa SG, Lopes RMC, Hu R, De Kleer
    K, Fisher C, Charnoz S, Baker AD, Halverson SP, Schneider NM, Psaridi A, Wyttenbach
    A, Torres Rodriguez S, Bhatnagar I, Johnson RE. 2024. Redshifted sodium transient
    near exoplanet transit. Astrophysical Journal Letters. 973(2), L53.
  mla: Oza, Apurva V., et al. “Redshifted Sodium Transient near Exoplanet Transit.”
    <i>Astrophysical Journal Letters</i>, vol. 973, no. 2, L53, IOP Publishing, 2024,
    doi:<a href="https://doi.org/10.3847/2041-8213/ad6b29">10.3847/2041-8213/ad6b29</a>.
  short: A.V. Oza, J.V. Seidel, H.J. Hoeijmakers, A. Unni, A.Y. Kesseli, C.A. Schmidt,
    T. Sivarani, A. Bello-Arufe, A. Gebek, M. Meyer Zu Westram, S.G. Sousa, R.M.C.
    Lopes, R. Hu, K. De Kleer, C. Fisher, S. Charnoz, A.D. Baker, S.P. Halverson,
    N.M. Schneider, A. Psaridi, A. Wyttenbach, S. Torres Rodriguez, I. Bhatnagar,
    R.E. Johnson, Astrophysical Journal Letters 973 (2024).
date_created: 2024-10-13T22:01:49Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:18:18Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/2041-8213/ad6b29
external_id:
  arxiv:
  - '2409.19844'
  isi:
  - '001322169500001'
file:
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  creator: dernst
  date_created: 2024-10-21T11:05:11Z
  date_updated: 2024-10-21T11:05:11Z
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has_accepted_license: '1'
intvolume: '       973'
isi: 1
issue: '2'
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
  eissn:
  - 2041-8213
  issn:
  - 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Redshifted sodium transient near exoplanet transit
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 973
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18528'
abstract:
- lang: eng
  text: The recent measurement of magnetic field strength inside the radiative interior
    of red giant stars has opened the way toward full 3D characterization of the geometry
    of stable large-scale magnetic fields. However, current measurements, which are
    limited to dipolar (ℓ = 1) mixed modes, do not properly constrain the topology
    of magnetic fields due to degeneracies on the observed magnetic field signature
    on such ℓ = 1 mode frequencies. Efforts focused toward unambiguous detections
    of magnetic field configurations are now key to better understand angular momentum
    transport in stars. We investigated the detectability of complex magnetic field
    topologies (such as the ones observed at the surface of stars with a radiative
    envelope with spectropolarimetry) inside the radiative interior of red giants.
    We focused on a field composed of a combination of a dipole and a quadrupole (quadrudipole)
    and on an offset field. We explored the potential of probing such magnetic field
    topologies from a combined measurement of magnetic signatures on ℓ = 1 and quadrupolar
    (ℓ = 2) mixed mode oscillation frequencies. We first derived the asymptotic theoretical
    formalism for computing the asymmetric signature in the frequency pattern for
    ℓ = 2 modes due to a quadrudipole magnetic field. To access asymmetry parameters
    for more complex magnetic field topologies, we numerically performed a grid search
    over the parameter space to map the degeneracy of the signatures of given topologies.
    We demonstrate the crucial role played by ℓ = 2 mixed modes in accessing internal
    magnetic fields with a quadrupolar component. The degeneracy of the quadrudipole
    compared to pure dipolar fields is lifted when considering magnetic asymmetries
    in both ℓ = 1 and ℓ = 2 mode frequencies. In addition to the analytical derivation
    for the quadrudipole, we present the prospect for complex magnetic field inversions
    using magnetic sensitivity kernels from standard perturbation analysis for forward
    modeling. Using this method, we explored the detectability of offset magnetic
    fields from ℓ = 1 and ℓ = 2 frequencies and demonstrate that offset fields may
    be mistaken for weak and centered magnetic fields, resulting in underestimating
    the magnetic field strength in stellar cores. We emphasize the need to characterize
    ℓ = 2 mixed-mode frequencies, (along with the currently characterized ℓ = 1 mixed
    modes), to unveil the higher-order components of the geometry of buried magnetic
    fields and to better constrain angular momentum transport inside stars.
acknowledgement: The authors thank S. Mathis, L. Barrault, S. Torres, A. Cristea,
  and K. M. Smith for very useful discussions. This project has received funding from
  the European Union’s Horizon 2020 research and innovation programme under the Marie
  Skłodowska-Curíe grant agreement No 101034413. The authors thank the anonymous referee
  for valuable comments and suggestions to improve the manuscript.
article_number: A217
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Srijan B
  full_name: Das, Srijan B
  id: 9ce7c423-dacf-11ed-8942-e09c6cb27149
  last_name: Das
  orcid: 0000-0003-0896-7972
- first_name: Lukas
  full_name: Einramhof, Lukas
  id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c
  last_name: Einramhof
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
citation:
  ama: Das SB, Einramhof L, Bugnet LA. Unveiling complex magnetic field configurations
    in red giant stars. <i>Astronomy and Astrophysics</i>. 2024;690. doi:<a href="https://doi.org/10.1051/0004-6361/202450918">10.1051/0004-6361/202450918</a>
  apa: Das, S. B., Einramhof, L., &#38; Bugnet, L. A. (2024). Unveiling complex magnetic
    field configurations in red giant stars. <i>Astronomy and Astrophysics</i>. EDP
    Sciences. <a href="https://doi.org/10.1051/0004-6361/202450918">https://doi.org/10.1051/0004-6361/202450918</a>
  chicago: Das, Srijan B, Lukas Einramhof, and Lisa Annabelle Bugnet. “Unveiling Complex
    Magnetic Field Configurations in Red Giant Stars.” <i>Astronomy and Astrophysics</i>.
    EDP Sciences, 2024. <a href="https://doi.org/10.1051/0004-6361/202450918">https://doi.org/10.1051/0004-6361/202450918</a>.
  ieee: S. B. Das, L. Einramhof, and L. A. Bugnet, “Unveiling complex magnetic field
    configurations in red giant stars,” <i>Astronomy and Astrophysics</i>, vol. 690.
    EDP Sciences, 2024.
  ista: Das SB, Einramhof L, Bugnet LA. 2024. Unveiling complex magnetic field configurations
    in red giant stars. Astronomy and Astrophysics. 690, A217.
  mla: Das, Srijan B., et al. “Unveiling Complex Magnetic Field Configurations in
    Red Giant Stars.” <i>Astronomy and Astrophysics</i>, vol. 690, A217, EDP Sciences,
    2024, doi:<a href="https://doi.org/10.1051/0004-6361/202450918">10.1051/0004-6361/202450918</a>.
  short: S.B. Das, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics 690 (2024).
corr_author: '1'
date_created: 2024-11-10T23:02:00Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:36:39Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202450918
ec_funded: 1
external_id:
  arxiv:
  - '2405.20133'
  isi:
  - '001336485200015'
file:
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  checksum: d43bbe6ed8ce4512e65e2d0d87070cf6
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has_accepted_license: '1'
intvolume: '       690'
isi: 1
language:
- iso: eng
month: '10'
oa: 1
oa_version: Published Version
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
  call_identifier: H2020
  grant_number: '101034413'
  name: 'IST-BRIDGE: International postdoctoral program'
publication: Astronomy and Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Unveiling complex magnetic field configurations in red giant stars
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18904'
abstract:
- lang: eng
  text: The Planetary Transits and Oscillations of stars mission (PLATO) will allow
    us to measure surface rotation and monitor photometric activity of tens of thousands
    of main sequence solar-type and subgiant stars. This paper is the first of a series
    dedicated to the preparation of the analysis of stellar surface rotation and photospheric
    activity with the near-future PLATO data. We describe in this work the strategy
    that will be implemented in the PLATO pipeline to measure stellar surface rotation,
    photometric activity, and long-term modulations. The algorithms are applied on
    both noise-free and noisy simulations of solar-type stars, which include activity
    cycles, latitudinal differential rotation, and spot evolution. PLATO simulated
    systematics are included in the noisy light curves. We show that surface rotation
    periods can be recovered with confidence for most of the stars with only six months
    of observations and that the recovery rate of the analysis significantly improves
    as additional observations are collected. This means that the first PLATO data
    release will already provide a substantial set of measurements for this quantity,
    with a significant refinement on their quality as the instrument obtains longer
    light curves. Measuring the Schwabe-like magnetic activity cycle during the mission
    will require that the same field be observed over a significant timescale (more
    than four years). Nevertheless, PLATO will provide a vast and robust sample of
    solar-type stars with constraints on the activity-cycle length. Such a sample
    is lacking from previous missions dedicated to space photometry.
acknowledgement: 'This work presents results from the European Space Agency (ESA)
  space mission PLATO. The PLATO payload, the PLATO Ground Segment and PLATO data
  processing are joint developments of ESA and the PLATO Mission Consortium (PMC).
  Funding for the PMC is provided at national levels, in particular by countries participating
  in the PLATO Multilateral Agreement (Austria, Belgium, Czech Republic, Denmark,
  France, Germany, Italy, Netherlands, Portugal, Spain, Sweden, Switzerland, Norway,
  and United Kingdom) and institutions from Brazil. Members of the PLATO Consortium
  can be found at https://platomission.com. The ESA PLATO mission website is https://www.cosmos.esa.int/plato.
  The authors thank the teams working for PLATO for all their work. They acknowledge
  the critical reading and the constructive comments from the anonymous referee that
  significantly allowed improving the original version of this paper. They finally
  thank R. Samadi for helpful advice and suggestions concerning the PSLS abilities.
  S.N.B, A.F.L, S.Me, I.P and E.C acknowledge support from PLATO ASI-INAF agreement
  no. 2022-28-HH.0 “PLATO Fase D”. S.N.B, L.A, A.S.B, Q.N, and A.S acknowledge financial
  support by ERC Whole Sun Synergy grant #810218. S.N.B, R.A.G, L.A, A.S.B, Q.N.,
  D.B.P, E.P, and A.S acknowledge the support from PLATO CNES grant. R.A.G, D.B.P,
  and E.P acknowledge the support from SoHO/GOLF CNES grant. A.S.B, Q.N, and A.S acknowledge
  the support from INSU/PNST grant and Solar Orbiter CNES grant. A.S acknowledges
  funding from from the European Union’s Horizon-2020 research and innovation program
  (grant agreement no. 776403 ExoplANETS-A) and the Programme National de Planétologie
  (PNP). A.R.G.S acknowledges the support from the FCT through national funds and
  FEDER through COMPETE2020 (UIDB/04434/2020, UIDP/04434/2020, 2022.03993.PTDC) and
  the support from the FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001.
  S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN)
  with the Ramón y Cajal fellowship no. RYC-2015-17697 and through AEI under the Severo
  Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.Ma acknowledges
  support from the Spanish Ministry of Science and Innovation (MICINN) with the grant
  no. PID2019-107187GB-I00. M.J.G., K.B., R.M.O, J.P, O.R., C.R. acknowledge support
  from CNES. The computations were performed with the IRFU/CEA Saclay server facilities,
  funded by ERC Synergy grant WholeSun No.810218, the P2IO Labex emergence project
  FlarePredict, and CNES PLATO funds. Software:star-privateer (this work), pyspot
  (Aigrain et al. 2015), PSLS (Samadi et al. 2019), numpy (Harris et al. 2020), matplotlib
  (Hunter 2007), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration 2022),
  pandas (Wes McKinney 2010; The pandas development team 2020), scikit-learn (Pedregosa
  et al. 2011).'
article_number: A229
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S. N.
  full_name: Breton, S. N.
  last_name: Breton
- first_name: A. F.
  full_name: Lanza, A. F.
  last_name: Lanza
- first_name: S.
  full_name: Messina, S.
  last_name: Messina
- first_name: I.
  full_name: Pagano, I.
  last_name: Pagano
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: E.
  full_name: Corsaro, E.
  last_name: Corsaro
- first_name: R. A.
  full_name: García, R. A.
  last_name: García
- first_name: S.
  full_name: Mathur, S.
  last_name: Mathur
- first_name: A. R. G.
  full_name: Santos, A. R. G.
  last_name: Santos
- first_name: S.
  full_name: Aigrain, S.
  last_name: Aigrain
- first_name: L.
  full_name: Amard, L.
  last_name: Amard
- first_name: A. S.
  full_name: Brun, A. S.
  last_name: Brun
- first_name: L.
  full_name: Degott, L.
  last_name: Degott
- first_name: Q.
  full_name: Noraz, Q.
  last_name: Noraz
- first_name: D. B.
  full_name: Palakkatharappil, D. B.
  last_name: Palakkatharappil
- first_name: E.
  full_name: Panetier, E.
  last_name: Panetier
- first_name: A.
  full_name: Strugarek, A.
  last_name: Strugarek
- first_name: K.
  full_name: Belkacem, K.
  last_name: Belkacem
- first_name: M.-J
  full_name: Goupil, M.-J
  last_name: Goupil
- first_name: R. M.
  full_name: Ouazzani, R. M.
  last_name: Ouazzani
- first_name: J.
  full_name: Philidet, J.
  last_name: Philidet
- first_name: C.
  full_name: Renié, C.
  last_name: Renié
- first_name: O.
  full_name: Roth, O.
  last_name: Roth
citation:
  ama: Breton SN, Lanza AF, Messina S, et al. Measuring stellar surface rotation and
    activity with the PLATO mission. I. Strategy and application to simulated light
    curves. <i>Astronomy and Astrophysics</i>. 2024;689. doi:<a href="https://doi.org/10.1051/0004-6361/202449893">10.1051/0004-6361/202449893</a>
  apa: Breton, S. N., Lanza, A. F., Messina, S., Pagano, I., Bugnet, L. A., Corsaro,
    E., … Roth, O. (2024). Measuring stellar surface rotation and activity with the
    PLATO mission. I. Strategy and application to simulated light curves. <i>Astronomy
    and Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202449893">https://doi.org/10.1051/0004-6361/202449893</a>
  chicago: Breton, S. N., A. F. Lanza, S. Messina, I. Pagano, Lisa Annabelle Bugnet,
    E. Corsaro, R. A. García, et al. “Measuring Stellar Surface Rotation and Activity
    with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.”
    <i>Astronomy and Astrophysics</i>. EDP Sciences, 2024. <a href="https://doi.org/10.1051/0004-6361/202449893">https://doi.org/10.1051/0004-6361/202449893</a>.
  ieee: S. N. Breton <i>et al.</i>, “Measuring stellar surface rotation and activity
    with the PLATO mission. I. Strategy and application to simulated light curves,”
    <i>Astronomy and Astrophysics</i>, vol. 689. EDP Sciences, 2024.
  ista: Breton SN, Lanza AF, Messina S, Pagano I, Bugnet LA, Corsaro E, García RA,
    Mathur S, Santos ARG, Aigrain S, Amard L, Brun AS, Degott L, Noraz Q, Palakkatharappil
    DB, Panetier E, Strugarek A, Belkacem K, Goupil M-J, Ouazzani RM, Philidet J,
    Renié C, Roth O. 2024. Measuring stellar surface rotation and activity with the
    PLATO mission. I. Strategy and application to simulated light curves. Astronomy
    and Astrophysics. 689, A229.
  mla: Breton, S. N., et al. “Measuring Stellar Surface Rotation and Activity with
    the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” <i>Astronomy
    and Astrophysics</i>, vol. 689, A229, EDP Sciences, 2024, doi:<a href="https://doi.org/10.1051/0004-6361/202449893">10.1051/0004-6361/202449893</a>.
  short: S.N. Breton, A.F. Lanza, S. Messina, I. Pagano, L.A. Bugnet, E. Corsaro,
    R.A. García, S. Mathur, A.R.G. Santos, S. Aigrain, L. Amard, A.S. Brun, L. Degott,
    Q. Noraz, D.B. Palakkatharappil, E. Panetier, A. Strugarek, K. Belkacem, M.-J.
    Goupil, R.M. Ouazzani, J. Philidet, C. Renié, O. Roth, Astronomy and Astrophysics
    689 (2024).
date_created: 2025-01-27T13:12:44Z
date_published: 2024-09-01T00:00:00Z
date_updated: 2025-09-09T12:04:24Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.1051/0004-6361/202449893
external_id:
  arxiv:
  - '2407.03709'
  isi:
  - '001366206400007'
file:
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  checksum: 5c871ba7370a507ed6ea9fb2304d8263
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  creator: dernst
  date_created: 2025-01-27T13:18:41Z
  date_updated: 2025-01-27T13:18:41Z
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intvolume: '       689'
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language:
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month: '09'
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oa_version: Published Version
publication: Astronomy and Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Measuring stellar surface rotation and activity with the PLATO mission. I.
  Strategy and application to simulated light curves
tmp:
  image: /images/cc_by.png
  legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
  name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
  short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 689
year: '2024'
...