[{"volume":2,"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"133-153","language":[{"iso":"eng"}],"title":"Asteroseismology","arxiv":1,"publication_status":"published","quality_controlled":"1","oa":1,"status":"public","OA_place":"repository","intvolume":"         2","author":[{"full_name":"Bowman, Dominic M.","first_name":"Dominic M.","last_name":"Bowman"},{"full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000"}],"editor":[{"first_name":"Ilya","full_name":"Mandel, Ilya","last_name":"Mandel"}],"department":[{"_id":"LiBu"}],"month":"01","year":"2026","OA_type":"green","type":"book_chapter","publication_identifier":{"isbn":["9780443214400"]},"day":"01","publisher":"Elsevier","publication":"Encyclopedia of Astrophysics","date_published":"2026-01-01T00:00:00Z","doi":"10.1016/b978-0-443-21439-4.00036-5","date_created":"2026-02-16T10:43:01Z","external_id":{"arxiv":["2410.01715"]},"citation":{"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>","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>.","ista":"Bowman DM, Bugnet LA. 2026.Asteroseismology. In: Encyclopedia of Astrophysics. vol. 2, 133–153.","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>.","short":"D.M. Bowman, L.A. Bugnet, in:, I. Mandel (Ed.), Encyclopedia of Astrophysics, Elsevier, 2026, pp. 133–153.","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>","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."},"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2410.01715","open_access":"1"}],"_id":"21230","article_processing_charge":"No","abstract":[{"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.","lang":"eng"}],"scopus_import":"1","date_updated":"2026-02-17T11:05:20Z"},{"doi":"10.1051/0004-6361/202659309","article_type":"letter_editor","date_created":"2026-04-05T22:01:32Z","external_id":{"arxiv":["2603.01979"]},"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.","_id":"21659","citation":{"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.","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>","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>.","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).","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>.","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>"},"article_processing_charge":"No","abstract":[{"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.","lang":"eng"}],"scopus_import":"1","date_updated":"2026-04-07T09:23:27Z","year":"2026","department":[{"_id":"LiBu"}],"month":"03","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"OA_type":"diamond","type":"journal_article","day":"01","publication":"Astronomy & Astrophysics","publisher":"Wiley","file":[{"file_name":"2026_AstronomyAstrophysics_Breton.pdf","creator":"dernst","relation":"main_file","file_size":1535506,"date_updated":"2026-04-07T09:20:02Z","content_type":"application/pdf","file_id":"21666","date_created":"2026-04-07T09:20:02Z","checksum":"a7fd798bf450d67d4166fdf54ff2c70c","access_level":"open_access","success":1}],"article_number":"L16","date_published":"2026-03-01T00:00:00Z","project":[{"_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631"}],"oa":1,"status":"public","ddc":["520"],"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","intvolume":"       707","has_accepted_license":"1","author":[{"last_name":"Breton","full_name":"Breton, S. N.","first_name":"S. N."},{"last_name":"Pezzotti","full_name":"Pezzotti, C.","first_name":"C."},{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Di Mauro","first_name":"M. P.","full_name":"Di Mauro, M. P."},{"last_name":"Joergensen","full_name":"Joergensen, J.","first_name":"J."},{"full_name":"Zwintz, K.","first_name":"K.","last_name":"Zwintz"},{"full_name":"Lanza, A. F.","first_name":"A. F.","last_name":"Lanza"}],"volume":707,"DOAJ_listed":"1","PlanS_conform":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"title":"Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars","publication_status":"published","file_date_updated":"2026-04-07T09:20:02Z","quality_controlled":"1"},{"oa":1,"ddc":["520"],"status":"public","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","intvolume":"      1001","issue":"2","has_accepted_license":"1","author":[{"last_name":"Pérez-Couto","first_name":"X.","full_name":"Pérez-Couto, X."},{"first_name":"Santiago","full_name":"Torres Rodriguez, Santiago","orcid":"0000-0002-3150-8988","last_name":"Torres Rodriguez","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2"},{"last_name":"Villaver","first_name":"E.","full_name":"Villaver, E."},{"full_name":"Mustill, A. J.","first_name":"A. J.","last_name":"Mustill"},{"full_name":"Manteiga, M.","first_name":"M.","last_name":"Manteiga"}],"DOAJ_listed":"1","volume":1001,"oa_version":"Published Version","PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"3I/ATLAS: In search of the witnesses to its voyage","arxiv":1,"file_date_updated":"2026-04-28T13:06:00Z","publication_status":"published","quality_controlled":"1","doi":"10.3847/1538-4357/ae56ff","external_id":{"arxiv":["2509.07678"]},"ec_funded":1,"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.","date_created":"2026-04-26T22:01:46Z","article_type":"original","citation":{"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>","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>","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.","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>.","short":"X. Pérez-Couto, S. Torres Rodriguez, E. Villaver, A.J. Mustill, M. Manteiga, The Astrophysical Journal 1001 (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>."},"_id":"21760","article_processing_charge":"Yes","abstract":[{"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.","lang":"eng"}],"scopus_import":"1","date_updated":"2026-04-28T13:08:39Z","department":[{"_id":"LiBu"}],"month":"04","year":"2026","OA_type":"gold","type":"journal_article","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"day":"20","file":[{"date_created":"2026-04-28T13:06:00Z","file_id":"21773","content_type":"application/pdf","success":1,"access_level":"open_access","checksum":"c3daf49261a9933c079854c38eec316f","file_name":"2026_AstrophysicalJournal_PerezCouto.pdf","date_updated":"2026-04-28T13:06:00Z","file_size":2905627,"creator":"dernst","relation":"main_file"}],"publisher":"IOP Publishing","publication":"The Astrophysical Journal","article_number":"146","project":[{"grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"date_published":"2026-04-20T00:00:00Z"},{"month":"03","department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"year":"2026","OA_type":"diamond","type":"journal_article","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"day":"01","article_number":"A321","date_published":"2026-03-01T00:00:00Z","file":[{"relation":"main_file","creator":"dernst","date_updated":"2026-04-07T09:00:50Z","file_size":12287607,"file_name":"2026_AstronomyAstrophysics_Liagre.pdf","checksum":"560cac19dc70184626b85e71a26ee22e","access_level":"open_access","success":1,"content_type":"application/pdf","file_id":"21664","date_created":"2026-04-07T09:00:50Z"}],"publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","external_id":{"arxiv":["2511.05314 "]},"date_created":"2026-04-05T22:01:32Z","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_type":"original","doi":"10.1051/0004-6361/202558023","article_processing_charge":"No","citation":{"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 &#38; 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 &#38; 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 &#38; Astrophysics 707 (2026).","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 &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>.","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 &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202558023\">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 &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","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 &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>"},"_id":"21658","abstract":[{"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.","lang":"eng"}],"date_updated":"2026-07-08T06:39:05Z","scopus_import":"1","oa_version":"Published Version","PlanS_conform":"1","DOAJ_listed":"1","volume":707,"corr_author":"1","title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"file_date_updated":"2026-04-07T09:00:50Z","publication_status":"published","quality_controlled":"1","oa":1,"OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"status":"public","ddc":["520"],"has_accepted_license":"1","intvolume":"       707","author":[{"first_name":"Bastien Raymond Bernard","full_name":"Liagre, Bastien Raymond Bernard","last_name":"Liagre","id":"662f1873-cab4-11f0-a719-8087d302868d"},{"id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","last_name":"Desai","full_name":"Desai, Aayush A","first_name":"Aayush A"},{"full_name":"Einramhof, Lukas","first_name":"Lukas","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","last_name":"Einramhof"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"}],"das_tickbox":"1"},{"oa_version":"Published Version","PlanS_conform":"1","DOAJ_listed":"1","volume":1005,"title":"Revealing mixed modes in compressible hydrodynamical simulations of red giant stars","arxiv":1,"keyword":["Stellar physics","Stellar interiors","Asteroseismology","Stellar oscillations","Hydrodynamical simulations"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"file_date_updated":"2026-07-13T08:14:01Z","publication_status":"published","quality_controlled":"1","oa":1,"supplementarymaterial":"yes","OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"ddc":["520"],"status":"public","has_accepted_license":"1","issue":"2","intvolume":"      1005","author":[{"first_name":"Nils B.","full_name":"De Vries, Nils B.","last_name":"De Vries"},{"last_name":"Le Saux","full_name":"Le Saux, Arthur","first_name":"Arthur"},{"first_name":"Isabelle","full_name":"Baraffe, Isabelle","last_name":"Baraffe"},{"last_name":"Guillet","full_name":"Guillet, Thomas","first_name":"Thomas"},{"last_name":"Townsend","full_name":"Townsend, Richard H.D.","first_name":"Richard H.D."},{"full_name":"Leclerc, Armand","first_name":"Armand","id":"2a1fb1fc-f373-11ef-901a-87cee43a1217","last_name":"Leclerc"},{"first_name":"Adrien","full_name":"Morison, Adrien","last_name":"Morison"}],"das_tickbox":"1","month":"07","department":[{"_id":"LiBu"}],"year":"2026","OA_type":"gold","type":"journal_article","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"day":"10","article_number":"154","date_published":"2026-07-10T00:00:00Z","project":[{"_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631"}],"publisher":"IOP Publishing","file":[{"date_updated":"2026-07-13T08:14:01Z","file_size":14866194,"relation":"main_file","creator":"dernst","file_name":"2026_AstrophysicalJour_deVries.pdf","success":1,"checksum":"d32061d2341bac3adeb404975c6bd59e","access_level":"open_access","file_id":"22275","date_created":"2026-07-13T08:14:01Z","content_type":"application/pdf"}],"publication":"The Astrophysical Journal","external_id":{"arxiv":["2606.07125"]},"acknowledgement":"We would like to thank the referee for their careful reading of the manuscript and their constructive comments that helped improve the paper. N.B.V. would like to thank K. Belkacem and J. Philidet for helpful discussions. N.B.V. is supported by STFC grant ST/Y002164/1. A.L.S. acknowledges 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 ATPS (CNRS/INSU). Part of this work was supported by the ERC grant No. 787361-COBOM. R.H.D.T. acknowledges support from NASA grants 80NSSC24K0895 and 80NSSC23K1517, and NSF grant 2407636. A.L. is supported by ERC Starting Grant 101165631 (“Calcifer”). The authors would like to acknowledge the use of the University of Exeter High-Performance Computing (HPC) facility, ISCA, in carrying out this work. This work used the DiRAC Memory Intensive service (Cosma8) at Durham University, managed by the Institute for Computational Cosmology, and the DiRAC Data Intensive service (DIaL3) at the University of Leicester, managed by the University of Leicester Research Computing Service. These facilities are managed on behalf of the STFC DiRAC HPC (www.dirac.ac.uk). The DiRAC services at Durham and Leicester were funded by BEIS, UKRI, and STFC capital funding, and STFC operations grants. The service at Durham received funding from Durham University. DiRAC is part of the UKRI Digital Research Infrastructure.","date_created":"2026-07-12T22:02:17Z","dataavailabilitystatement":"The kinetic energies and surface velocities shown in Figure 4, as well as the underlying spectral data of this work, can be found in a Zenodo repository at doi:10.5281/zenodo.18661976.","article_type":"original","doi":"10.3847/1538-4357/ae7a3c","article_processing_charge":"Yes","citation":{"apa":"De Vries, N. B., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D., Leclerc, A., &#38; Morison, A. (2026). Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>","ista":"De Vries NB, Le Saux A, Baraffe I, Guillet T, Townsend RHD, Leclerc A, Morison A. 2026. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. 1005(2), 154.","mla":"De Vries, Nils B., et al. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>, vol. 1005, no. 2, 154, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>.","chicago":"De Vries, Nils B., Arthur Le Saux, Isabelle Baraffe, Thomas Guillet, Richard H.D. Townsend, Armand Leclerc, and Adrien Morison. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">https://doi.org/10.3847/1538-4357/ae7a3c</a>.","short":"N.B. De Vries, A. Le Saux, I. Baraffe, T. Guillet, R.H.D. Townsend, A. Leclerc, A. Morison, The Astrophysical Journal 1005 (2026).","ama":"De Vries NB, Le Saux A, Baraffe I, et al. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. <i>The Astrophysical Journal</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7a3c\">10.3847/1538-4357/ae7a3c</a>","ieee":"N. B. De Vries <i>et al.</i>, “Revealing mixed modes in compressible hydrodynamical simulations of red giant stars,” <i>The Astrophysical Journal</i>, vol. 1005, no. 2. IOP Publishing, 2026."},"_id":"22262","abstract":[{"text":"Mixed modes are observed in many low-mass evolved stars. They provide information about core rotation rates of these stars, which are lower than predicted by stellar evolution models. The mixed modes themselves have been invoked as an angular momentum (AM) transport mechanism, but estimating their transport efficiency requires knowledge of their amplitudes. We constrain, for the first time, the mixed-mode amplitudes in 2D hydrodynamical simulations of a 1.3M⊙ red giant using the code MUSIC. We perform two simulations with outer radial truncations at fractional radii ro/r⋆ = 0.90 and 0.98. We compare the modes in the simulation with those found using both GYRE and a Dedalus eigenvalue solver. Excellent frequency agreement is found for all p-dominated modes, with minor discrepancies for g-dominated modes, especially in the frequency range [60, 240] μHz. We find excellent eigenfunction agreement for all modes except those in this frequency range. According to empirical predictions, the largest kinetic energies are located around Vmax= 312.μHz, but in both simulations, the modes with frequencies of ν < 50 μHz have the largest kinetic energies. In the simulation with r/r⋆ = 0.98, the simulated modes have extrapolated surface velocities comparable to the empirical predictions, with the highest surface velocities in a bell-shaped curve peaking around ν = 700 μHz. The extrapolated surface velocities of the low-frequency modes are small and thus hard to observe, but their large kinetic energies deeper in the interior could significantly impact AM transport, which has not yet been investigated.","lang":"eng"}],"researchdata_availability":"yes","date_updated":"2026-07-13T08:16:25Z","scopus_import":"1"},{"oa":1,"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","ddc":["520"],"status":"public","has_accepted_license":"1","intvolume":"       704","author":[{"full_name":"Gragera-Más, J. L.","first_name":"J. L.","last_name":"Gragera-Más"},{"first_name":"Santiago","full_name":"Torres Rodriguez, Santiago","last_name":"Torres Rodriguez","orcid":"0000-0002-3150-8988","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2"},{"last_name":"Mustill","first_name":"A. J.","full_name":"Mustill, A. J."},{"last_name":"Villaver","full_name":"Villaver, E.","first_name":"E."}],"oa_version":"Published Version","PlanS_conform":"1","volume":704,"DOAJ_listed":"1","arxiv":1,"title":"A kinematic history of stellar encounters with Beta Pictoris","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","file_date_updated":"2026-01-05T11:06:16Z","quality_controlled":"1","article_type":"original","external_id":{"arxiv":["2510.02509"]},"ec_funded":1,"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.","date_created":"2026-01-04T23:01:34Z","doi":"10.1051/0004-6361/202555940","article_processing_charge":"No","_id":"20930","citation":{"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>","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).","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>.","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>","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."},"abstract":[{"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.","lang":"eng"}],"date_updated":"2026-02-16T12:15:07Z","scopus_import":"1","year":"2025","department":[{"_id":"LiBu"}],"month":"12","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"type":"journal_article","OA_type":"diamond","day":"01","article_number":"A237","project":[{"grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"date_published":"2025-12-01T00:00:00Z","publication":"Astronomy & Astrophysics","file":[{"file_size":11021467,"date_updated":"2026-01-05T11:06:16Z","creator":"dernst","relation":"main_file","file_name":"2025_AstronomyAstrophysics_GrageraMas.pdf","success":1,"checksum":"2fb4d5a1603043aa7931a31f2c180877","access_level":"open_access","file_id":"20942","date_created":"2026-01-05T11:06:16Z","content_type":"application/pdf"}],"publisher":"EDP Sciences"},{"file":[{"checksum":"b8a0927307c1d82025bcb5af47b20b26","access_level":"open_access","success":1,"content_type":"application/pdf","file_id":"21306","date_created":"2026-02-17T13:07:45Z","relation":"main_file","creator":"dernst","file_size":7161755,"date_updated":"2026-02-17T13:07:45Z","file_name":"2025_AstronomyAstrophysics_Bessila.pdf"}],"publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","date_published":"2025-08-01T00:00:00Z","article_number":"A25","day":"01","type":"journal_article","OA_type":"gold","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"month":"08","department":[{"_id":"LiBu"}],"year":"2025","date_updated":"2026-02-17T13:10:18Z","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."}],"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>","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.","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>.","short":"L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A. García, S. Mathur, Astronomy &#38; Astrophysics 700 (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>.","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>"},"_id":"21252","article_processing_charge":"Yes","doi":"10.1051/0004-6361/202452093","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).","date_created":"2026-02-16T15:46:59Z","article_type":"original","quality_controlled":"1","file_date_updated":"2026-02-17T13:07:45Z","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators","DOAJ_listed":"1","volume":700,"oa_version":"Published Version","PlanS_conform":"1","author":[{"full_name":"Bessila, L.","first_name":"L.","last_name":"Bessila"},{"last_name":"Deckx van Ruys","first_name":"A.","full_name":"Deckx van Ruys, A."},{"first_name":"V.","full_name":"Buriasco, V.","last_name":"Buriasco"},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"last_name":"García","full_name":"García, R. A.","first_name":"R. A."},{"first_name":"S.","full_name":"Mathur, S.","last_name":"Mathur"}],"intvolume":"       700","has_accepted_license":"1","status":"public","ddc":["520"],"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","oa":1},{"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2512.15170","open_access":"1"}],"citation":{"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>","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>.","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.","ieee":"J. Vandersnickt <i>et al.</i>, “Expanding stellar horizons with polarized light,” <i>arXiv</i>. .","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>","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>.","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.)."},"_id":"21309","status":"public","article_processing_charge":"No","OA_place":"repository","oa":1,"doi":"10.48550/arXiv.2512.15170","external_id":{"arxiv":["2512.15170"]},"date_created":"2026-02-17T13:53:50Z","author":[{"last_name":"Vandersnickt","first_name":"J.","full_name":"Vandersnickt, J."},{"first_name":"R. Ochoa","full_name":"Armenta, R. Ochoa","last_name":"Armenta"},{"last_name":"Vanlaer","first_name":"V.","full_name":"Vanlaer, V."},{"last_name":"A. David-Uraz","first_name":"A. David-Uraz","full_name":"A. David-Uraz, A. David-Uraz"},{"first_name":"C.","full_name":"Aerts, C.","last_name":"Aerts"},{"full_name":"Das, S. B.","first_name":"S. B.","last_name":"Das"},{"last_name":"Bouret","first_name":"J. -C.","full_name":"Bouret, J. -C."},{"last_name":"Bowman","first_name":"D. M.","full_name":"Bowman, D. M."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle"},{"last_name":"Khalack","full_name":"Khalack, V.","first_name":"V."},{"full_name":"J. Labadie-Bartz, J. Labadie-Bartz","first_name":"J. Labadie-Bartz","last_name":"J. Labadie-Bartz"},{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"last_name":"Nazé","full_name":"Nazé, Y.","first_name":"Y."},{"last_name":"Neiner","first_name":"C.","full_name":"Neiner, C."},{"last_name":"Petit","full_name":"Petit, P.","first_name":"P."},{"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"},{"last_name":"Doorsselaere","first_name":"T. Van","full_name":"Doorsselaere, T. Van"},{"last_name":"Vanrespaille","full_name":"Vanrespaille, M.","first_name":"M."}],"date_updated":"2026-04-07T06:00:40Z","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."}],"OA_type":"green","type":"preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"Expanding stellar horizons with polarized light","arxiv":1,"department":[{"_id":"LiBu"}],"month":"12","year":"2025","oa_version":"Preprint","publication":"arXiv","article_number":"2512.15170","date_published":"2025-12-17T00:00:00Z","publication_status":"submitted","day":"17"},{"publication":"Monthly Notices of the Royal Astronomical Society","file":[{"content_type":"application/pdf","file_id":"20881","date_created":"2025-12-30T07:24:34Z","checksum":"49fb4fe69f487d36169ccea60acbeccc","access_level":"open_access","success":1,"file_name":"2025_MonthlyNoticesRAS_Xing.pdf","relation":"main_file","creator":"dernst","date_updated":"2025-12-30T07:24:34Z","file_size":2974244}],"publisher":"Oxford University Press","project":[{"call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413"}],"date_published":"2025-02-01T00:00:00Z","day":"01","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"OA_type":"gold","type":"journal_article","year":"2025","month":"02","department":[{"_id":"YlGo"},{"_id":"LiBu"}],"scopus_import":"1","date_updated":"2025-12-30T07:25:37Z","abstract":[{"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.","lang":"eng"}],"_id":"18984","citation":{"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>","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.","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.","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>.","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>","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>."},"article_processing_charge":"Yes","doi":"10.1093/mnras/stae2820","article_type":"original","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.","external_id":{"arxiv":["2410.19695"],"isi":["001400731500001"]},"ec_funded":1,"date_created":"2025-02-02T23:01:53Z","quality_controlled":"1","publication_status":"published","file_date_updated":"2025-12-30T07:24:34Z","page":"285-292","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"title":"Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries","volume":537,"DOAJ_listed":"1","oa_version":"Published Version","PlanS_conform":"1","author":[{"full_name":"Xing, Zepei","first_name":"Zepei","last_name":"Xing"},{"last_name":"Torres Rodriguez","orcid":"0000-0002-3150-8988","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","first_name":"Santiago","full_name":"Torres Rodriguez, Santiago"},{"first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"last_name":"Trani","first_name":"Alessandro A.","full_name":"Trani, Alessandro A."},{"full_name":"Korol, Valeriya","first_name":"Valeriya","last_name":"Korol"},{"last_name":"Cuadra","first_name":"Jorge","full_name":"Cuadra, Jorge"}],"intvolume":"       537","issue":"1","has_accepted_license":"1","ddc":["520"],"status":"public","OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"isi":1,"oa":1},{"author":[{"first_name":"Lucas","full_name":"Barrault, Lucas","last_name":"Barrault","id":"4471a8fd-32c1-11ee-a9a4-fb670d398f64"},{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"}],"intvolume":"       694","has_accepted_license":"1","ddc":["520"],"status":"public","isi":1,"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","oa":1,"quality_controlled":"1","file_date_updated":"2025-03-04T09:57:03Z","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"Constraining differential rotation in γ Doradus stars from the properties of inertial dips","corr_author":"1","volume":694,"oa_version":"Published Version","scopus_import":"1","date_updated":"2026-02-16T12:09:14Z","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."}],"citation":{"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>","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.","short":"L. Barrault, S. Mathis, L.A. Bugnet, Astronomy &#38; Astrophysics 694 (2025).","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>","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>.","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>."},"_id":"19283","article_processing_charge":"Yes","doi":"10.1051/0004-6361/202451541","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.","date_created":"2025-03-02T23:01:53Z","external_id":{"isi":["001424452400025"]},"article_type":"original","publisher":"EDP Sciences","file":[{"checksum":"568a5e5951f20483663df145a780fc3d","access_level":"open_access","success":1,"content_type":"application/pdf","file_id":"19288","date_created":"2025-03-04T09:57:03Z","relation":"main_file","creator":"dernst","file_size":7438476,"date_updated":"2025-03-04T09:57:03Z","file_name":"2025_AstronomyAstrophysics_Barrault.pdf"}],"publication":"Astronomy & Astrophysics","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631"}],"article_number":"A225","date_published":"2025-02-01T00:00:00Z","day":"01","type":"journal_article","OA_type":"diamond","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"department":[{"_id":"LiBu"}],"month":"02","year":"2025"},{"intvolume":"       276","issue":"2","has_accepted_license":"1","author":[{"first_name":"Marc H.","full_name":"Pinsonneault, Marc H.","last_name":"Pinsonneault"},{"last_name":"Zinn","full_name":"Zinn, Joel C.","first_name":"Joel C."},{"last_name":"Tayar","first_name":"Jamie","full_name":"Tayar, Jamie"},{"first_name":"Aldo","full_name":"Serenelli, Aldo","last_name":"Serenelli"},{"full_name":"García, Rafael A.","first_name":"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"},{"last_name":"Mosser","full_name":"Mosser, Benoit","first_name":"Benoit"},{"full_name":"Stello, Dennis","first_name":"Dennis","last_name":"Stello"},{"full_name":"Bell, Keaton J.","first_name":"Keaton J.","last_name":"Bell"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle"},{"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"},{"last_name":"Huber","first_name":"Daniel","full_name":"Huber, Daniel"},{"first_name":"Thomas","full_name":"Kallinger, Thomas","last_name":"Kallinger"},{"last_name":"Cao","full_name":"Cao, Kaili","first_name":"Kaili"},{"last_name":"Johnson","first_name":"Jennifer A.","full_name":"Johnson, Jennifer A."},{"full_name":"Liagre, Bastien","first_name":"Bastien","last_name":"Liagre"},{"last_name":"Patton","full_name":"Patton, Rachel A.","first_name":"Rachel A."},{"last_name":"Santos","full_name":"Santos, Ângela R.G.","first_name":"Ângela R.G."},{"full_name":"Basu, Sarbani","first_name":"Sarbani","last_name":"Basu"},{"full_name":"Beck, Paul G.","first_name":"Paul G.","last_name":"Beck"},{"last_name":"Beers","first_name":"Timothy C.","full_name":"Beers, Timothy C."},{"full_name":"Chaplin, William J.","first_name":"William J.","last_name":"Chaplin"},{"first_name":"Katia","full_name":"Cunha, Katia","last_name":"Cunha"},{"last_name":"Frinchaboy","full_name":"Frinchaboy, Peter M.","first_name":"Peter M."},{"last_name":"Girardi","first_name":"Léo","full_name":"Girardi, Léo"},{"first_name":"Diego","full_name":"Godoy-Rivera, Diego","last_name":"Godoy-Rivera"},{"last_name":"Holtzman","first_name":"Jon A.","full_name":"Holtzman, Jon A."},{"first_name":"Henrik","full_name":"Jönsson, Henrik","last_name":"Jönsson"},{"first_name":"Szabolcs","full_name":"Mészáros, Szabolcs","last_name":"Mészáros"},{"full_name":"Reyes, Claudia","first_name":"Claudia","last_name":"Reyes"},{"last_name":"Rix","full_name":"Rix, Hans Walter","first_name":"Hans Walter"},{"last_name":"Shetrone","full_name":"Shetrone, Matthew","first_name":"Matthew"},{"full_name":"Smith, Verne V.","first_name":"Verne V.","last_name":"Smith"},{"last_name":"Spoo","full_name":"Spoo, Taylor","first_name":"Taylor"},{"last_name":"Stassun","full_name":"Stassun, Keivan G.","first_name":"Keivan G."},{"last_name":"Wang","full_name":"Wang, Ji","first_name":"Ji"}],"oa":1,"ddc":["520"],"status":"public","isi":1,"OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file_date_updated":"2025-03-17T10:40:41Z","publication_status":"published","quality_controlled":"1","DOAJ_listed":"1","volume":276,"oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"title":"APOKASC-3: The third joint spectroscopic and asteroseismic catalog for evolved stars in the Kepler fields","arxiv":1,"abstract":[{"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.","lang":"eng"}],"scopus_import":"1","date_updated":"2025-09-30T11:03:01Z","doi":"10.3847/1538-4365/ad9fef","external_id":{"arxiv":["2410.00102"],"isi":["001414132600001"]},"date_created":"2025-03-16T23:01:24Z","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_type":"original","citation":{"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>","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).","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.","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>","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>.","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."},"_id":"19405","article_processing_charge":"Yes","day":"01","file":[{"relation":"main_file","creator":"dernst","file_size":4993506,"date_updated":"2025-03-17T10:40:41Z","file_name":"2025_AstrophysicalJourSuppl_Pinsonneault.pdf","access_level":"open_access","checksum":"a01a6645c6cb0b5cc75490f3339a2244","success":1,"content_type":"application/pdf","date_created":"2025-03-17T10:40:41Z","file_id":"19414"}],"publisher":"IOP Publishing","publication":"Astrophysical Journal, Supplement Series","date_published":"2025-02-01T00:00:00Z","article_number":"69","month":"02","department":[{"_id":"LiBu"}],"year":"2025","type":"journal_article","OA_type":"gold","publication_identifier":{"issn":["0067-0049"]}},{"author":[{"last_name":"Rauer","first_name":"Heike","full_name":"Rauer, Heike"},{"last_name":"Aerts","full_name":"Aerts, Conny","first_name":"Conny"},{"first_name":"Juan","full_name":"Cabrera, Juan","last_name":"Cabrera"},{"last_name":"Deleuil","full_name":"Deleuil, Magali","first_name":"Magali"},{"last_name":"Erikson","full_name":"Erikson, Anders","first_name":"Anders"},{"full_name":"Gizon, Laurent","first_name":"Laurent","last_name":"Gizon"},{"first_name":"Mariejo","full_name":"Goupil, Mariejo","last_name":"Goupil"},{"last_name":"Heras","full_name":"Heras, Ana","first_name":"Ana"},{"last_name":"Walloschek","first_name":"Thomas","full_name":"Walloschek, Thomas"},{"full_name":"Lorenzo-Alvarez, Jose","first_name":"Jose","last_name":"Lorenzo-Alvarez"},{"first_name":"Filippo","full_name":"Marliani, Filippo","last_name":"Marliani"},{"last_name":"Martin-Garcia","first_name":"César","full_name":"Martin-Garcia, César"},{"first_name":"J. Miguel","full_name":"Mas-Hesse, J. Miguel","last_name":"Mas-Hesse"},{"last_name":"O’Rourke","full_name":"O’Rourke, Laurence","first_name":"Laurence"},{"full_name":"Osborn, Hugh","first_name":"Hugh","last_name":"Osborn"},{"last_name":"Pagano","first_name":"Isabella","full_name":"Pagano, Isabella"},{"first_name":"Giampaolo","full_name":"Piotto, Giampaolo","last_name":"Piotto"},{"last_name":"Pollacco","first_name":"Don","full_name":"Pollacco, Don"},{"first_name":"Roberto","full_name":"Ragazzoni, Roberto","last_name":"Ragazzoni"},{"last_name":"Ramsay","full_name":"Ramsay, Gavin","first_name":"Gavin"},{"last_name":"Udry","first_name":"Stéphane","full_name":"Udry, Stéphane"},{"last_name":"Appourchaux","first_name":"Thierry","full_name":"Appourchaux, Thierry"},{"full_name":"Benz, Willy","first_name":"Willy","last_name":"Benz"},{"full_name":"Brandeker, Alexis","first_name":"Alexis","last_name":"Brandeker"},{"first_name":"Manuel","full_name":"Güdel, Manuel","last_name":"Güdel"},{"first_name":"Eduardo","full_name":"Janot-Pacheco, 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Kempen","first_name":"Tim A.","full_name":"Van Kempen, Tim A."},{"full_name":"Van Reeth, Timothy","first_name":"Timothy","last_name":"Van Reeth"},{"last_name":"Van Zelst","first_name":"Iris","full_name":"Van Zelst, Iris"},{"full_name":"Vandenbussche, Bart","first_name":"Bart","last_name":"Vandenbussche"},{"first_name":"Konstantinos","full_name":"Vasiliou, Konstantinos","last_name":"Vasiliou"},{"last_name":"Vasilyev","full_name":"Vasilyev, Valeriy","first_name":"Valeriy"},{"last_name":"Vaz De Mascarenhas","first_name":"David","full_name":"Vaz De Mascarenhas, David"},{"first_name":"Allona","full_name":"Vazan, Allona","last_name":"Vazan"},{"full_name":"Vela Nunez, Marina","first_name":"Marina","last_name":"Vela Nunez"},{"full_name":"Velloso, Eduardo Nunes","first_name":"Eduardo Nunes","last_name":"Velloso"},{"full_name":"Ventura, Rita","first_name":"Rita","last_name":"Ventura"},{"first_name":"Paolo","full_name":"Ventura, Paolo","last_name":"Ventura"},{"full_name":"Venturini, 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Annita"},{"last_name":"Wendler","first_name":"Belinda","full_name":"Wendler, Belinda"},{"full_name":"West, Richard","first_name":"Richard","last_name":"West"},{"first_name":"Karsten","full_name":"Westerdorff, Karsten","last_name":"Westerdorff"},{"first_name":"Pierre Amaury","full_name":"Westphal, Pierre Amaury","last_name":"Westphal"},{"first_name":"Peter","full_name":"Wheatley, Peter","last_name":"Wheatley"},{"last_name":"White","full_name":"White, Tim","first_name":"Tim"},{"last_name":"Whittaker","full_name":"Whittaker, Amadou","first_name":"Amadou"},{"last_name":"Wickhusen","full_name":"Wickhusen, Kai","first_name":"Kai"},{"last_name":"Wilson","full_name":"Wilson, Thomas","first_name":"Thomas"},{"full_name":"Windsor, James","first_name":"James","last_name":"Windsor"},{"last_name":"Winter","first_name":"Othon","full_name":"Winter, Othon"},{"full_name":"Winther, Mark Lykke","first_name":"Mark Lykke","last_name":"Winther"},{"full_name":"Winton, Alistair","first_name":"Alistair","last_name":"Winton"},{"last_name":"Witteck","first_name":"Ulrike","full_name":"Witteck, Ulrike"},{"last_name":"Witzke","first_name":"Veronika","full_name":"Witzke, Veronika"},{"last_name":"Woitke","full_name":"Woitke, Peter","first_name":"Peter"},{"full_name":"Wolter, David","first_name":"David","last_name":"Wolter"},{"first_name":"Günther","full_name":"Wuchterl, Günther","last_name":"Wuchterl"},{"last_name":"Wyatt","full_name":"Wyatt, Mark","first_name":"Mark"},{"last_name":"Yang","full_name":"Yang, Dan","first_name":"Dan"},{"full_name":"Yu, Jie","first_name":"Jie","last_name":"Yu"},{"last_name":"Zanmar Sanchez","full_name":"Zanmar Sanchez, Ricardo","first_name":"Ricardo"},{"last_name":"Zapatero Osorio","first_name":"María Rosa","full_name":"Zapatero Osorio, María Rosa"},{"first_name":"Mathias","full_name":"Zechmeister, Mathias","last_name":"Zechmeister"},{"first_name":"Yixiao","full_name":"Zhou, Yixiao","last_name":"Zhou"},{"last_name":"Ziemke","first_name":"Claas","full_name":"Ziemke, Claas"},{"full_name":"Zwintz, Konstanze","first_name":"Konstanze","last_name":"Zwintz"},{"last_name":"Böhm","full_name":"Böhm, Torsten","first_name":"Torsten"},{"last_name":"Dansac","full_name":"Dansac, Léo Michel","first_name":"Léo Michel"}],"intvolume":"        59","issue":"3","has_accepted_license":"1","ddc":["520"],"status":"public","isi":1,"OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"oa":1,"quality_controlled":"1","file_date_updated":"2025-05-05T10:42:05Z","publication_status":"published","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","language":[{"iso":"eng"}],"title":"The PLATO mission","volume":59,"oa_version":"Published Version","scopus_import":"1","date_updated":"2026-04-02T11:44:00Z","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."}],"citation":{"ieee":"H. Rauer <i>et al.</i>, “The PLATO mission,” <i>Experimental Astronomy</i>, vol. 59, no. 3. Springer Nature, 2025.","chicago":"Rauer, Heike, Conny Aerts, Juan Cabrera, Magali Deleuil, Anders Erikson, Laurent Gizon, Mariejo Goupil, et al. “The PLATO Mission.” <i>Experimental Astronomy</i>. Springer Nature, 2025. <a href=\"https://doi.org/10.1007/s10686-025-09985-9\">https://doi.org/10.1007/s10686-025-09985-9</a>.","short":"H. Rauer, C. Aerts, J. Cabrera, M. Deleuil, A. Erikson, L. Gizon, M. Goupil, A. Heras, T. Walloschek, J. Lorenzo-Alvarez, F. Marliani, C. Martin-Garcia, J.M. Mas-Hesse, L. O’Rourke, H. Osborn, I. Pagano, G. Piotto, D. Pollacco, R. Ragazzoni, G. Ramsay, S. Udry, T. Appourchaux, W. Benz, A. Brandeker, M. Güdel, E. Janot-Pacheco, P. Kabath, H. Kjeldsen, M. Min, N. Santos, A. Smith, J.C. Suarez, S.C. Werner, A. Aboudan, M. Abreu, L. Acuña, M. Adams, V. Adibekyan, L. Affer, F. Agneray, C. Agnor, V. Aguirre Børsen-Koch, S. Ahmed, S. Aigrain, A. Al-Bahlawan, M.D.L.A. Alcacera Gil, E. Alei, S. Alencar, R. Alexander, J. Alfonso-Garzón, Y. Alibert, C. Allende Prieto, L. Almeida, R. Alonso Sobrino, G. Altavilla, C. Althaus, L.A. Alvarez Trujillo, A. Amarsi, M. Ammler-Von Eiff, E. Amôres, L. Andrade, A. Antoniadis-Karnavas, C. António, B. Aparicio Del Moral, M. Appolloni, C. Arena, D. Armstrong, J. Aroca Aliaga, M. Asplund, J. Audenaert, N. Auricchio, P. Avelino, A. Baeke, K. Baillié, A. Balado, P. Ballber Balagueró, A. Balestra, W. Ball, H. Ballans, J. Ballot, C. Barban, G. Barbary, M. Barbieri, S. Barceló Forteza, A. Barker, P. Barklem, S. Barnes, D. Barrado Navascues, O. Barragan, C. Baruteau, S. Basu, F. Baudin, P. Baumeister, D. Bayliss, M. Bazot, P.G. Beck, K. Belkacem, E. Bellinger, S. Benatti, O. Benomar, D. Bérard, M. Bergemann, M. Bergomi, P. Bernardo, K. Biazzo, A. Bignamini, L. Bigot, N. Billot, M. Binet, D. Biondi, F. Biondi, A.C. Birch, B. Bitsch, P.V. Bluhm Ceballos, A. Bódi, Z. Bognár, I. Boisse, E. Bolmont, A. Bonanno, M. Bonavita, A. Bonfanti, X. Bonfils, R. Bonito, A.S. Bonomo, A. Börner, S. Boro Saikia, E. Borreguero Martín, F. Borsa, L. Borsato, D. Bossini, F. Bouchy, G. Boué, R. Boufleur, P. Boumier, V. Bourrier, D.M. Bowman, E. Bozzo, L. Bradley, J. Bray, A. Bressan, S. Breton, D. Brienza, A. Brito, M. Brogi, B. Brown, D.J.A. Brown, A.S. Brun, G. Bruno, M. Bruns, L.A. Buchhave, L.A. Bugnet, G. Buldgen, P. Burgess, A. Busatta, G. Busso, D. Buzasi, J.A. Caballero, A. Cabral, J.F. Cabrero Gomez, F. Calderone, R. Cameron, A. Cameron, T. Campante, N. Campos Gestal, B.L. Canto Martins, C. Cara, L. Carone, J.M. Carrasco, L. Casagrande, S.L. Casewell, S. Cassisi, M. Castellani, M. Castro, C. Catala, I. Catalán Fernández, M. Catelan, H. Cegla, C. Cerruti, V. Cessa, M. Chadid, W. Chaplin, S. Charpinet, C. Chiappini, S. Chiarucci, A. Chiavassa, S. Chinellato, G. Chirulli, J. Christensen-Dalsgaard, R. Church, A. Claret, C. Clarke, R. Claudi, L. Clermont, H. Coelho, J. Coelho, F. Cogato, J. Colomé, M. Condamin, F. Conde García, S. Conseil, T. Corbard, A.C.M. Correia, E. Corsaro, R. Cosentino, J. Costes, A. Cottinelli, G. Covone, O.L. Creevey, A. Crida, S. Csizmadia, M. Cunha, P. Curry, J. Da Costa, F. Da Silva, S. Dalal, M. Damasso, C. Damiani, F. Damiani, M.L. Das Chagas, M. Davies, G. Davies, B. Davies, G. Davison, L. De Almeida, F. De Angeli, S.C.C. De Barros, I. De Castroleão, D.B. De Freitas, M.C. De Freitas, D. De Martino, J.R. De Medeiros, L.A. De Paula, Á. De Pedraza Gómez, J. De Plaa, J. De Ridder, M. Deal, L. Decin, H. Deeg, S. Degl’Innocenti, S. Deheuvels, C. Del Burgo, F. Del Sordo, E. Delgado-Mena, O. Demangeon, T. Denk, A. Derekas, J.M. Desert, S. Desidera, M. Dexet, M. Di Criscienzo, A.M. Di Giorgio, M.P. Di Mauro, F.J. Diaz Rial, J.J. Díaz-García, M. Dima, G. Dinuzzi, O. Dionatos, E. Distefano, J.D. Do Nascimento, A. Domingo, V. D’Orazi, C. Dorn, L. Doyle, E. Duarte, F. Ducellier, L. Dumaye, X. Dumusque, M.A. Dupret, P. Eggenberger, D. Ehrenreich, P. Eigmüller, J. Eising, M. Emilio, K. Eriksson, M. Ermocida, R.I. Escate Giribaldi, Y. Eschen, L. Espinosa Yáñez, I. Estrela, D.W. Evans, D. Fabbian, M. Fabrizio, J.P. Faria, M. Farina, J. Farinato, D. Feliz, S. Feltzing, T. Fenouillet, M. Fernández, L. Ferrari, S. Ferraz-Mello, F. Fialho, A. Fienga, P. Figueira, L. Fiori, E. Flaccomio, M. Focardi, S. Foley, J. Fontignie, D. Ford, K. Fornazier, T. Forveille, L. Fossati, R.D.M. Franca, L. Franco Da Silva, A. Frasca, M. Fridlund, M. Furlan, S.M. Gabler, M. Gaido, A. Gallagher, P.I. Gallego Sempere, E. Galli, R.A. García, A. García Hernández, A. Garcia Munoz, H. García-Vázquez, R. Garrido Haba, P. Gaulme, N. Gauthier, C. Gehan, M. Gent, I. Georgieva, M. Ghigo, E. Giana, S. Gill, L. Girardi, S. Giuliatti Winter, G. Giusi, J. Gomes Da Silva, L.J. Gómez Zazo, J.M. Gomez-Lopez, J.I. González Hernández, K. Gonzalez Murillo, A. Gonzalo Melchor, N. Gorius, P.V. Gouel, D. Goulty, V. Granata, J.L. Grenfell, D. Grießbach, E. Grolleau, S. Grouffal, S. Grziwa, M.G. Guarcello, L. Gueguen, E.W. Guenther, T. Guilhem, L. Guillerot, T. Guillot, P. Guiot, P. Guterman, A. Gutiérrez, F. Gutiérrez-Canales, J. Hagelberg, J. Haldemann, C. Hall, R. Handberg, I. Harrison, D.L. Harrison, J. Hasiba, C.A. Haswell, P. Hatalova, A. Hatzes, R. Haywood, G. Hébrard, F. Heckes, U. Heiter, S. Hekker, R. Heller, C. Helling, K. Helminiak, S. Hemsley, K. Heng, K. Herbst, A. Hermans, J.J. Hermes, N. Hidalgo Torres, N. Hinkel, D. Hobbs, S. Hodgkin, K. Hofmann, S. Hojjatpanah, G. Houdek, 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. Mahy, O. Maibaum, L.R. Malac-Allain, J.C. Malapert, L. Malavolta, J. Maldonado, E. Mamonova, L. Manchon, A. Manjón, A. Mann, G. Mantovan, L. Marafatto, M. Marconi, R. Mardling, P. Marigo, S. Marinoni, R. Marques, J.P. Marques, P.M. Marrese, D. Marshall, S. Martínez Perales, D. Mary, F. Marzari, E. Masana, A. Mascher, S. Mathis, S. Mathur, I. Martín Vodopivec, A.C. Mattiuci Figueiredo, P.F.L. Maxted, T. Mazeh, S. Mazevet, F. Mazzei, J. Mccormac, P. Mcmillan, L. Menou, T. Merle, F. Meru, D. Mesa, S. Messina, S. Mészáros, N. Meunier, J.C. Meunier, G. Micela, 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, J. Montalban, M. Montalto, M.J.P.F.G. Monteiro, F. Montoro Sánchez, J.C. Morales, M. Morales-Calderon, A. Morbidelli, C. Mordasini, C. Moreau, T. Morel, G. Morello, J. Morin, A. Mortier, B. Mosser, D. Mourard, O. Mousis, C. Moutou, N. Mowlavi, A. Moya, P. Muehlmann, P. Muirhead, M. Munari, I. Musella, A.J. Mustill, N. Nardetto, D. Nardiello, N. Narita, V. Nascimbeni, A. Nash, C. Neiner, R.P. Nelson, N. Nettelmann, G. Nicolini, M. Nielsen, S.M. Niemi, L. Noack, A. Noels-Grotsch, A. Noll, A. Norazman, A.J. Norton, B. Nsamba, A. Ofir, G. Ogilvie, T. Olander, C. Olivetto, G. Olofsson, 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, V. Parro, H. Parviainen, J. Pascual Granado, V.M. Passegger, C. Pastor-Morales, M. Pätzold, M.G. Pedersen, D. Pena Hidalgo, F. Pepe, F. Pereira, C.M. Persson, 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, G. Ramos Zapata, S. Rätz, C. Rauterberg, B. Redman, R. Redmer, D. Reese, S. Regibo, A. Reiners, T. Reinhold, C. Renie, I. Ribas, S. Ribeiro, T.P. Ricciardi, K. Rice, O. Richard, M. Riello, M. Rieutord, V. Ripepi, G. Rixon, S. Rockstein, J.R. Rodón 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).","ama":"Rauer H, Aerts C, Cabrera J, et al. The PLATO mission. <i>Experimental Astronomy</i>. 2025;59(3). doi:<a href=\"https://doi.org/10.1007/s10686-025-09985-9\">10.1007/s10686-025-09985-9</a>","mla":"Rauer, Heike, et al. “The PLATO Mission.” <i>Experimental Astronomy</i>, vol. 59, no. 3, 26, Springer Nature, 2025, doi:<a href=\"https://doi.org/10.1007/s10686-025-09985-9\">10.1007/s10686-025-09985-9</a>.","ista":"Rauer H et al. 2025. The PLATO mission. Experimental Astronomy. 59(3), 26.","apa":"Rauer, H., Aerts, C., Cabrera, J., Deleuil, M., Erikson, A., Gizon, L., … Dansac, L. M. (2025). The PLATO mission. <i>Experimental Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1007/s10686-025-09985-9\">https://doi.org/10.1007/s10686-025-09985-9</a>"},"_id":"19637","article_processing_charge":"Yes (via OA deal)","doi":"10.1007/s10686-025-09985-9","external_id":{"isi":["001498306700001"]},"acknowledgement":"Open Access funding enabled and organized by Projekt DEAL.","date_created":"2025-05-04T22:02:30Z","article_type":"original","file":[{"content_type":"application/pdf","file_id":"19652","date_created":"2025-05-05T10:42:05Z","checksum":"e2c21a3d7ae1438b2061eb0fc95e63b7","access_level":"open_access","success":1,"file_name":"2025_ExperimentalAstronomy_Rauer.pdf","creator":"dernst","relation":"main_file","date_updated":"2025-05-05T10:42:05Z","file_size":6305300}],"publisher":"Springer Nature","publication":"Experimental Astronomy","date_published":"2025-04-21T00:00:00Z","article_number":"26","day":"21","type":"journal_article","OA_type":"hybrid","publication_identifier":{"eissn":["1572-9508"],"issn":["0922-6435"]},"department":[{"_id":"LiBu"}],"month":"04","year":"2025"},{"department":[{"_id":"GradSch"},{"_id":"LiBu"}],"month":"10","year":"2025","type":"dissertation","publication_identifier":{"issn":["2791-4585"]},"day":"08","date_published":"2025-10-08T00:00:00Z","alternative_title":["ISTA Master's Thesis"],"publisher":"Institute of Science and Technology Austria","file":[{"creator":"ksmith","relation":"source_file","date_updated":"2025-10-08T09:45:33Z","file_size":8263624,"file_name":"2025_Smith_Kanah_Thesis.zip","checksum":"80d241d11b69af771c1fab0998be4f19","access_level":"closed","content_type":"application/zip","file_id":"20434","date_created":"2025-10-08T08:01:42Z"},{"success":1,"checksum":"13cb48cc98e00fdfe32f3ff66f17aa26","access_level":"open_access","file_id":"20439","date_created":"2025-10-09T14:38:57Z","content_type":"application/pdf","date_updated":"2025-10-09T14:38:57Z","file_size":9748339,"relation":"main_file","creator":"ksmith","file_name":"2025_Smith_Kanah_Thesis.pdf"}],"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","date_created":"2025-06-20T13:27:08Z","doi":"10.15479/AT-ISTA-19853","article_processing_charge":"No","citation":{"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>.","ista":"Smith K. 2025. Exploring internal magnetism in partially suppressed red giant stars. Institute of Science and Technology Austria.","ieee":"K. Smith, “Exploring internal magnetism in partially suppressed red giant stars,” Institute of Science and Technology Austria, 2025.","short":"K. Smith, Exploring Internal Magnetism in Partially Suppressed Red Giant Stars, Institute of Science and Technology Austria, 2025.","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>","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>.","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>"},"degree_awarded":"MS","_id":"19853","abstract":[{"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.","lang":"eng"}],"date_updated":"2026-04-07T12:01:37Z","oa_version":"Published Version","corr_author":"1","title":"Exploring internal magnetism in partially suppressed red giant stars","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","keyword":["asteroseismology","stellar physics","red giant","magnetism","suppressed"],"page":"38","language":[{"iso":"eng"}],"file_date_updated":"2025-10-09T14:38:57Z","publication_status":"published","oa":1,"supervisor":[{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"}],"OA_place":"publisher","ddc":["520"],"status":"public","has_accepted_license":"1","author":[{"full_name":"Smith, Kanah","first_name":"Kanah","id":"7703505d-3211-11ee-a6a9-a2ab9d936c15","last_name":"Smith"}]},{"type":"journal_article","OA_type":"diamond","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"department":[{"_id":"LiBu"}],"month":"09","year":"2025","file":[{"creator":"dernst","relation":"main_file","date_updated":"2025-09-15T06:58:09Z","file_size":3175077,"file_name":"2025_AstronomyAstrophysics_Vanlaer.pdf","checksum":"9ee9f34cf86305602d6cb3e07a1cc1a6","access_level":"open_access","success":1,"content_type":"application/pdf","file_id":"20354","date_created":"2025-09-15T06:58:09Z"}],"publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","article_number":"A5","project":[{"grant_number":"101034413","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program"},{"grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"date_published":"2025-09-01T00:00:00Z","day":"01","citation":{"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>","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>.","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>","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.","short":"V. Vanlaer, D.M. Bowman, S. Burssens, S.B. Das, L.A. Bugnet, S. Mathis, C. Aerts, Astronomy &#38; Astrophysics 701 (2025).","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>."},"_id":"20350","article_processing_charge":"No","doi":"10.1051/0004-6361/202452885","external_id":{"isi":["001561561200007"],"arxiv":["2506.19948"]},"ec_funded":1,"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.","date_created":"2025-09-14T22:01:32Z","article_type":"original","scopus_import":"1","date_updated":"2026-02-16T12:12:53Z","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."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries","arxiv":1,"volume":701,"PlanS_conform":"1","oa_version":"Published Version","quality_controlled":"1","file_date_updated":"2025-09-15T06:58:09Z","publication_status":"published","status":"public","ddc":["520"],"isi":1,"OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"oa":1,"author":[{"first_name":"V.","full_name":"Vanlaer, V.","last_name":"Vanlaer"},{"last_name":"Bowman","full_name":"Bowman, D. M.","first_name":"D. M."},{"last_name":"Burssens","full_name":"Burssens, S.","first_name":"S."},{"last_name":"Das","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","full_name":"Das, Srijan B"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"S.","full_name":"Mathis, S.","last_name":"Mathis"},{"last_name":"Aerts","first_name":"C.","full_name":"Aerts, C."}],"intvolume":"       701","has_accepted_license":"1"},{"doi":"10.1051/0004-6361/202555213","article_type":"original","external_id":{"arxiv":["2507.00308"],"isi":["001585834500002"]},"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.","date_created":"2025-10-12T22:01:26Z","_id":"20454","citation":{"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>","short":"L. Barrault, L.A. Bugnet, S. Mathis, J.S.G. Mombarg, Astronomy &#38; Astrophysics 701 (2025).","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>.","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>","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.","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>.","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."},"article_processing_charge":"No","abstract":[{"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.","lang":"eng"}],"scopus_import":"1","date_updated":"2026-02-19T09:32:04Z","year":"2025","month":"09","department":[{"_id":"LiBu"},{"_id":"GradSch"}],"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"OA_type":"diamond","type":"journal_article","day":"01","publication":"Astronomy & Astrophysics","file":[{"relation":"main_file","creator":"dernst","file_size":2503149,"date_updated":"2025-10-13T07:05:55Z","file_name":"2025_AstronomyAstrophysics_BarraultL.pdf","access_level":"open_access","checksum":"2c209b33119af4a251bab4a418a21075","success":1,"content_type":"application/pdf","date_created":"2025-10-13T07:05:55Z","file_id":"20459"}],"publisher":"EDP Sciences","project":[{"grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"article_number":"A253","date_published":"2025-09-01T00:00:00Z","oa":1,"ddc":["520"],"status":"public","OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"isi":1,"intvolume":"       701","has_accepted_license":"1","author":[{"id":"4471a8fd-32c1-11ee-a9a4-fb670d398f64","last_name":"Barrault","full_name":"Barrault, Lucas","first_name":"Lucas"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"last_name":"Mombarg","first_name":"J. S.G.","full_name":"Mombarg, J. S.G."}],"volume":701,"oa_version":"Published Version","PlanS_conform":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"corr_author":"1","title":"Exploring the probing power of γ Dor's inertial dip for core magnetism: The case of a toroidal field","publication_status":"published","file_date_updated":"2025-10-13T07:05:55Z","quality_controlled":"1"},{"publication_status":"published","file_date_updated":"2026-01-05T08:36:28Z","quality_controlled":"1","volume":704,"DOAJ_listed":"1","oa_version":"Published Version","PlanS_conform":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields","intvolume":"       704","has_accepted_license":"1","author":[{"last_name":"Mombarg","full_name":"Mombarg, J. S.G.","first_name":"J. S.G."},{"first_name":"V.","full_name":"Vanlaer, V.","last_name":"Vanlaer"},{"first_name":"Srijan B","full_name":"Das, Srijan B","last_name":"Das","orcid":"0000-0003-0896-7972","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149"},{"last_name":"Rieutord","first_name":"M.","full_name":"Rieutord, M."},{"first_name":"C.","full_name":"Aerts, C.","last_name":"Aerts"},{"full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"last_name":"Reese","full_name":"Reese, D. R.","first_name":"D. R."},{"full_name":"Ballot, J.","first_name":"J.","last_name":"Ballot"}],"oa":1,"ddc":["520"],"status":"public","OA_place":"publisher","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"day":"19","publication":"Astronomy & Astrophysics","publisher":"EDP Sciences","file":[{"file_size":2620909,"date_updated":"2026-01-05T08:36:28Z","relation":"main_file","creator":"dernst","file_name":"2025_AstronomyAstrophysics_Mombarg.pdf","success":1,"access_level":"open_access","checksum":"d838b4783920c43b7cc866e9cf08b383","date_created":"2026-01-05T08:36:28Z","file_id":"20937","content_type":"application/pdf"}],"project":[{"name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020","grant_number":"101034413"},{"grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"date_published":"2025-12-19T00:00:00Z","article_number":"A336","year":"2025","month":"12","department":[{"_id":"LiBu"}],"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"OA_type":"diamond","type":"journal_article","abstract":[{"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.","lang":"eng"}],"scopus_import":"1","related_material":{"record":[{"relation":"research_data","status":"public","id":"20936"}]},"date_updated":"2026-07-22T06:20:53Z","doi":"10.1051/0004-6361/202557247","article_type":"original","ec_funded":1,"external_id":{"arxiv":["2511.09617"]},"date_created":"2026-01-04T23:01:35Z","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.","_id":"20931","citation":{"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>.","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).","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>","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.","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>.","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."},"article_processing_charge":"No"},{"ddc":["520"],"_id":"20936","status":"public","main_file_link":[{"url":"https://doi.org/10.5281/zenodo.17580178","open_access":"1"}],"citation":{"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>","short":"J. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S. Mathis, D. Reese, J. Ballot, (2025).","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>.","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>","ieee":"J. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?” Zenodo, 2025.","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>.","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>."},"OA_place":"repository","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"No","doi":"10.5281/ZENODO.17580178","oa":1,"date_created":"2026-01-05T08:39:33Z","related_material":{"record":[{"id":"20931","relation":"used_in_publication","status":"public"}]},"date_updated":"2026-07-22T06:20:53Z","author":[{"last_name":"Mombarg","first_name":"Joey","full_name":"Mombarg, Joey"},{"first_name":"Vincent","full_name":"Vanlaer, Vincent","last_name":"Vanlaer"},{"orcid":"0000-0003-0896-7972","last_name":"Das","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","full_name":"Das, Srijan B"},{"last_name":"Rieutord","full_name":"Rieutord, Michel","first_name":"Michel"},{"last_name":"Aerts","full_name":"Aerts, Conny","first_name":"Conny"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Mathis","first_name":"Stephane","full_name":"Mathis, Stephane"},{"last_name":"Reese","full_name":"Reese, Daniel","first_name":"Daniel"},{"full_name":"Ballot, Jerome","first_name":"Jerome","last_name":"Ballot"}],"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)"}],"OA_type":"gold","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"research_data_reference","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?","year":"2025","department":[{"_id":"LiBu"}],"month":"11","oa_version":"Published Version","publisher":"Zenodo","date_published":"2025-11-11T00:00:00Z","day":"11"},{"publication":"Nature Astronomy","publisher":"Springer Nature","project":[{"call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413"}],"date_published":"2024-09-01T00:00:00Z","day":"01","publication_identifier":{"eissn":["2397-3366"]},"type":"journal_article","OA_type":"closed access","year":"2024","month":"09","department":[{"_id":"LiBu"}],"scopus_import":"1","date_updated":"2025-09-08T08:04:56Z","abstract":[{"lang":"eng","text":"Supergranules, which are solar flow features with a lateral scale of 30,000–40,000 km and a lifetime of ~24 h, form a prominent component of the Sun’s convective spectrum. However, their internal flows, which can be probed only by helioseismology, are not well understood. We analyse dopplergrams recorded by the Solar Dynamics Observatory satellite to identify and characterize ~23,000 supergranules. We find that the vertical flows peak at a depth of ~10,000 km, and remain invariant over the full range of lateral supergranular scales, contrary to numerical predictions. We also infer that, within the local seismic resolution (≳5,000 km), downflows are ~40% weaker than upflows, indicating an apparent mass-flux imbalance. This may imply that the descending flows also comprise plumes, which maintain the mass balance but are simply too small to be detected by seismic waves. These results challenge the widely used mixing-length description of solar convection."}],"_id":"17189","citation":{"ista":"Hanson CS, Das SB, Mani P, Hanasoge S, Sreenivasan KR. 2024. Supergranular-scale solar convection not explained by mixing-length theory. Nature Astronomy. 8, 1088–1101.","mla":"Hanson, Chris S., et al. “Supergranular-Scale Solar Convection Not Explained by Mixing-Length Theory.” <i>Nature Astronomy</i>, vol. 8, Springer Nature, 2024, pp. 1088–101, doi:<a href=\"https://doi.org/10.1038/s41550-024-02304-w\">10.1038/s41550-024-02304-w</a>.","ieee":"C. S. Hanson, S. B. Das, P. Mani, S. Hanasoge, and K. R. Sreenivasan, “Supergranular-scale solar convection not explained by mixing-length theory,” <i>Nature Astronomy</i>, vol. 8. Springer Nature, pp. 1088–1101, 2024.","chicago":"Hanson, Chris S., Srijan B Das, Prasad Mani, Shravan Hanasoge, and Katepalli R. Sreenivasan. “Supergranular-Scale Solar Convection Not Explained by Mixing-Length Theory.” <i>Nature Astronomy</i>. Springer Nature, 2024. <a href=\"https://doi.org/10.1038/s41550-024-02304-w\">https://doi.org/10.1038/s41550-024-02304-w</a>.","short":"C.S. Hanson, S.B. Das, P. Mani, S. Hanasoge, K.R. Sreenivasan, Nature Astronomy 8 (2024) 1088–1101.","ama":"Hanson CS, Das SB, Mani P, Hanasoge S, Sreenivasan KR. Supergranular-scale solar convection not explained by mixing-length theory. <i>Nature Astronomy</i>. 2024;8:1088-1101. doi:<a href=\"https://doi.org/10.1038/s41550-024-02304-w\">10.1038/s41550-024-02304-w</a>","apa":"Hanson, C. S., Das, S. B., Mani, P., Hanasoge, S., &#38; Sreenivasan, K. R. (2024). Supergranular-scale solar convection not explained by mixing-length theory. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-024-02304-w\">https://doi.org/10.1038/s41550-024-02304-w</a>"},"article_processing_charge":"No","doi":"10.1038/s41550-024-02304-w","article_type":"original","ec_funded":1,"date_created":"2024-06-30T22:01:05Z","acknowledgement":"We thank F. J. Simons for the codes for computing Slepian functions,\r\nM. Rempel and R. Cameron for their insights into solar convection, J.\r\nW. Lord for the numerical simulations and J. Naranjo for his help with\r\nthe NYUAD NetDRMS system. This research was carried out with the\r\nHigh Performance Computing resources at NYUAD. The datasets were\r\nprepared in the data centre at the Center for Space Science of NYUAD.\r\nThis research is based upon work supported by Tamkeen under the\r\nNYUAD Research Institute (Grant Nos G1502 and CASS to C.S.H,\r\nS.H. and K.R.S.). S.H. acknowledges funding from the Department\r\nof Atomic Energy, India. K.R.S. and S.H. acknowledge support from\r\nthe Ofice of Sponsored Research of King Abdullah University of\r\nScience and Technology (Award No. OSR-CRG2020-4342). S.B.D.\r\nacknowledges funding from the Elisabeth H. and F. A. Dahlen Award\r\n2022 by the Department of Geosciences, Princeton University. S.B.D.\r\nalso acknowledges funding from the European Union’s Horizon 2020\r\nresearch and innovation programme under a Marie Skłodowska-Curie\r\ngrant (Grant Agreement No. 101034413). Some data products were\r\nprocessed and downloaded from the German Data Center for SDO,\r\nwhich is funded by the German Aerospace Center (DLR Grant No.\r\n500L1701).","external_id":{"isi":["001254181700001"]},"quality_controlled":"1","publication_status":"published","language":[{"iso":"eng"}],"page":"1088-1101","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Supergranular-scale solar convection not explained by mixing-length theory","volume":8,"oa_version":"None","author":[{"first_name":"Chris S.","full_name":"Hanson, Chris S.","last_name":"Hanson"},{"id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","orcid":"0000-0003-0896-7972","last_name":"Das","full_name":"Das, Srijan B","first_name":"Srijan B"},{"last_name":"Mani","first_name":"Prasad","full_name":"Mani, Prasad"},{"full_name":"Hanasoge, Shravan","first_name":"Shravan","last_name":"Hanasoge"},{"last_name":"Sreenivasan","first_name":"Katepalli R.","full_name":"Sreenivasan, Katepalli R."}],"intvolume":"         8","status":"public","isi":1},{"day":"15","date_published":"2024-07-15T00:00:00Z","project":[{"_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413"}],"article_number":"42","publisher":"IOP Publishing","file":[{"date_created":"2024-07-29T11:02:48Z","file_id":"17340","content_type":"application/pdf","success":1,"access_level":"open_access","checksum":"acb42a87deecbc9228fbbe6a48a37ec6","file_name":"2024_AstrophysicalJourn_Bhattacharya.pdf","date_updated":"2024-07-29T11:02:48Z","file_size":3912290,"relation":"main_file","creator":"dernst"}],"publication":"Astrophysical Journal","month":"07","department":[{"_id":"LiBu"}],"year":"2024","type":"journal_article","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"abstract":[{"lang":"eng","text":"Magnetic fields in the stellar interiors are key candidates to explain observed core rotation rates inside solar-like stars along their evolution. Recently, asteroseismic estimates of radial magnetic field amplitudes near the hydrogen-burning shell (H-shell) inside about 24 red giants (RGs) have been obtained by measuring frequency splittings from their power spectra. Using general Lorentz-stress (magnetic) kernels, we investigated the potential for detectability of near-surface magnetism in a 1.3 M⊙ star of supersolar metallicity as it evolves from a mid subgiant to a late subgiant into an RG. Based on these sensitivity kernels, we decompose an RG into three zones—deep core, H-shell, and near-surface. The subgiants instead required decomposition into an inner core, an outer core, and a near-surface layer. Additionally, we find that for a low-frequency g-dominated dipolar mode in the presence of a typical stable magnetic field, ∼25% of the frequency shift comes from the H-shell and the remaining from deeper layers. The ratio of the subsurface tangential field to the radial field in the H-burning shell decides if subsurface fields may be potentially detectable. For p-dominated dipole modes close to vmax, this ratio is around two orders of magnitude smaller in subgiant phases than the corresponding RG. Further, with the availability of magnetic kernels, we propose lower limits of field strengths in crucial layers in our stellar model during its evolutionary phases. The theoretical prescription outlined here provides the first formal way to devise inverse problems for stellar magnetism and can be seamlessly employed for slow rotators."}],"date_updated":"2025-09-08T08:42:20Z","scopus_import":"1","external_id":{"arxiv":["2404.17167"],"isi":["001270972500001"]},"ec_funded":1,"date_created":"2024-07-28T22:01:09Z","acknowledgement":"This project has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413. S.\r\nB.D. acknowledges Prof. Jeroen Tromp at Princeton University for supporting a part of this work. S.M.H., S.B., and S.P. acknowledge support from the Department of Atomic Energy,\r\nGovernment of India, under Project Identification No. RTI 4002. The authors would like to thank the reviewer(s) and data editor for their constructive comments and suggestions. The\r\ngeneration of the stellar models was done using the Modules for Experiments in Stellar Astrophysics (MESA Paxton et al. 2011, 2013, 2015, 2018, 2019; we have used MESA version\r\nr22.05.1 for RG and r23.05.1 for SG models, MESA-SDK version x86_64-linux-22.6.1). The eigenfrequencies and eigenfunctions for this model were calculated using the GYRE\r\n(Townsend & Teitler 2013) code. The code to calculate the kernels and the splittings has been written completely in Python 3.8.16.","article_type":"original","doi":"10.3847/1538-4357/ad4708","article_processing_charge":"Yes","citation":{"apa":"Bhattacharya, S., Das, S. B., Bugnet, L. A., Panda, S., &#38; Hanasoge, S. M. (2024). Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad4708\">https://doi.org/10.3847/1538-4357/ad4708</a>","ista":"Bhattacharya S, Das SB, Bugnet LA, Panda S, Hanasoge SM. 2024. Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. Astrophysical Journal. 970(1), 42.","mla":"Bhattacharya, Shatanik, et al. “Detectability of Axisymmetric Magnetic Fields from the Core to the Surface of Oscillating Post-Main-Sequence Stars.” <i>Astrophysical Journal</i>, vol. 970, no. 1, 42, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad4708\">10.3847/1538-4357/ad4708</a>.","ieee":"S. Bhattacharya, S. B. Das, L. A. Bugnet, S. Panda, and S. M. Hanasoge, “Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars,” <i>Astrophysical Journal</i>, vol. 970, no. 1. IOP Publishing, 2024.","short":"S. Bhattacharya, S.B. Das, L.A. Bugnet, S. Panda, S.M. Hanasoge, Astrophysical Journal 970 (2024).","chicago":"Bhattacharya, Shatanik, Srijan B Das, Lisa Annabelle Bugnet, Subrata Panda, and Shravan M. Hanasoge. “Detectability of Axisymmetric Magnetic Fields from the Core to the Surface of Oscillating Post-Main-Sequence Stars.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad4708\">https://doi.org/10.3847/1538-4357/ad4708</a>.","ama":"Bhattacharya S, Das SB, Bugnet LA, Panda S, Hanasoge SM. Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars. <i>Astrophysical Journal</i>. 2024;970(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad4708\">10.3847/1538-4357/ad4708</a>"},"_id":"17326","file_date_updated":"2024-07-29T11:02:48Z","publication_status":"published","quality_controlled":"1","oa_version":"Published Version","DOAJ_listed":"1","volume":970,"title":"Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main-sequence stars","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"has_accepted_license":"1","intvolume":"       970","issue":"1","author":[{"first_name":"Shatanik","full_name":"Bhattacharya, Shatanik","last_name":"Bhattacharya"},{"full_name":"Das, Srijan B","first_name":"Srijan B","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","last_name":"Das","orcid":"0000-0003-0896-7972"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Panda","full_name":"Panda, Subrata","first_name":"Subrata"},{"full_name":"Hanasoge, Shravan M.","first_name":"Shravan M.","last_name":"Hanasoge"}],"oa":1,"isi":1,"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"ddc":["520"],"status":"public"},{"scopus_import":"1","date_updated":"2025-09-08T09:53:01Z","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."}],"citation":{"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.","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>","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.","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>.","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>"},"_id":"18172","article_processing_charge":"Yes","doi":"10.1093/mnras/stae2053","date_created":"2024-10-06T22:01:11Z","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).","external_id":{"isi":["001320536900011"],"arxiv":["2409.01157"]},"article_type":"original","publisher":"Oxford University Press","file":[{"success":1,"access_level":"open_access","checksum":"b79f3c6a5991516abbcc8d34fa4bfb5f","date_created":"2024-10-07T09:14:03Z","file_id":"18182","content_type":"application/pdf","date_updated":"2024-10-07T09:14:03Z","file_size":2813008,"creator":"dernst","relation":"main_file","file_name":"2024_MonthlyNRoyalAstronSoc_Hatt.pdf"}],"publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2024-10-01T00:00:00Z","day":"01","type":"journal_article","OA_type":"gold","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"10","department":[{"_id":"LiBu"}],"year":"2024","author":[{"full_name":"Hatt, Emily J.","first_name":"Emily J.","last_name":"Hatt"},{"last_name":"Ong","first_name":"J. M.Joel","full_name":"Ong, J. M.Joel"},{"last_name":"Nielsen","first_name":"Martin B.","full_name":"Nielsen, Martin B."},{"full_name":"Chaplin, William J.","first_name":"William J.","last_name":"Chaplin"},{"last_name":"Davies","first_name":"Guy R.","full_name":"Davies, Guy R."},{"last_name":"Deheuvels","full_name":"Deheuvels, Sébastien","first_name":"Sébastien"},{"full_name":"Ballot, Jérôme","first_name":"Jérôme","last_name":"Ballot"},{"first_name":"Gang","full_name":"Li, Gang","last_name":"Li"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"}],"intvolume":"       534","issue":"2","has_accepted_license":"1","status":"public","ddc":["520"],"isi":1,"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","oa":1,"quality_controlled":"1","file_date_updated":"2024-10-07T09:14:03Z","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"1060-1076","language":[{"iso":"eng"}],"title":"Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants","arxiv":1,"DOAJ_listed":"1","volume":534,"oa_version":"Published Version","PlanS_conform":"1"}]