[{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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.","ddc":["520"],"oa":1,"publisher":"IOP Publishing","has_accepted_license":"1","supplementarymaterial":"yes","_id":"22262","date_updated":"2026-07-13T08:16:25Z","status":"public","article_processing_charge":"Yes","department":[{"_id":"LiBu"}],"intvolume":"      1005","oa_version":"Published Version","language":[{"iso":"eng"}],"external_id":{"arxiv":["2606.07125"]},"keyword":["Stellar physics","Stellar interiors","Asteroseismology","Stellar oscillations","Hydrodynamical simulations"],"volume":1005,"year":"2026","researchdata_availability":"yes","project":[{"grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"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"}],"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.","file":[{"creator":"dernst","date_created":"2026-07-13T08:14:01Z","date_updated":"2026-07-13T08:14:01Z","file_size":14866194,"success":1,"file_name":"2026_AstrophysicalJour_deVries.pdf","content_type":"application/pdf","file_id":"22275","checksum":"d32061d2341bac3adeb404975c6bd59e","access_level":"open_access","relation":"main_file"}],"issue":"2","quality_controlled":"1","title":"Revealing mixed modes in compressible hydrodynamical simulations of red giant stars","DOAJ_listed":"1","publication":"The Astrophysical Journal","arxiv":1,"citation":{"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).","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>.","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.","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>","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.","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>","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>."},"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae7a3c","article_number":"154","month":"07","author":[{"first_name":"Nils B.","last_name":"De Vries","full_name":"De Vries, Nils B."},{"full_name":"Le Saux, Arthur","last_name":"Le Saux","first_name":"Arthur"},{"last_name":"Baraffe","first_name":"Isabelle","full_name":"Baraffe, Isabelle"},{"last_name":"Guillet","first_name":"Thomas","full_name":"Guillet, Thomas"},{"full_name":"Townsend, Richard H.D.","first_name":"Richard H.D.","last_name":"Townsend"},{"full_name":"Leclerc, Armand","first_name":"Armand","last_name":"Leclerc","id":"2a1fb1fc-f373-11ef-901a-87cee43a1217"},{"last_name":"Morison","first_name":"Adrien","full_name":"Morison, Adrien"}],"date_created":"2026-07-12T22:02:17Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","das_tickbox":"1","OA_place":"publisher","PlanS_conform":"1","fulldoi":"https://doi.org/10.3847/1538-4357/ae7a3c","day":"10","OA_type":"gold","scopus_import":"1","file_date_updated":"2026-07-13T08:14:01Z","date_published":"2026-07-10T00:00:00Z","article_type":"original","publication_status":"published"},{"acknowledgement":"The authors thank the referee for their helpful and constructive report, which has significantly enhanced the quality of the manuscript.\r\nThe authors thank I. Caiazzo, L. Ferrario, and L. Buchele for very useful discussions. L. Barrault, L. Bugnet, and L. Einramhof gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe\r\nprogramme (Calcifer; Starting Grant agreement N◦101165631). L. Barrault\r\nacknowledges the support of the Austrian Academy of Sciences through the Doctoral Fellowship Programme (DOC) of the Austrian Academy of Sciences 27648.\r\nWhile partially funded by the European Union, views and opinions expressed\r\nare, 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\r\nnor the granting authority can be held responsible for them.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","ddc":["520"],"oa":1,"has_accepted_license":"1","supplementarymaterial":"yes","publisher":"EDP Sciences","department":[{"_id":"LiBu"},{"_id":"GradSch"}],"intvolume":"       708","_id":"22663","article_processing_charge":"No","date_updated":"2026-08-11T05:49:20Z","status":"public","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"},{"name":"Unveiling the structure and dynamics of the deep convective core - radiative zone boundary throughout stellar evolution","grant_number":"27648","_id":"5b62812b-ab3d-11f0-914f-8f3a9cdb4af7"}],"file":[{"file_id":"22671","content_type":"application/pdf","checksum":"61edee776603d7b879b06b3ea8d2bc89","access_level":"open_access","relation":"main_file","creator":"dernst","date_updated":"2026-08-11T05:46:02Z","date_created":"2026-08-11T05:46:02Z","file_size":3739424,"success":1,"file_name":"2026_AstronomyAstrophysics_Einramhof.pdf"}],"corr_author":"1","dataavailabilitystatement":"We used MESA version 24.08.1. All inlists and relevant files are available on Zenodo at https://doi.org/10.5281/zenodo.19232789","abstract":[{"lang":"eng","text":"The detection of strong, large-scale magnetic fields at the surfaces of the oldest white dwarfs might point toward a hidden internal magnetic field slowly rising to the surface. In addition, strong magnetic fields have recently been measured through asteroseismology in the radiative interiors of red giant stars, the progenitors of white dwarfs. To investigate the potential connection between these observations, we revisited the fossil field framework using asteroseismic detections to constrain the strength of such magnetic fields as red giants evolve into the white dwarf stage. We assumed that the magnetic field was either created during the core convection on the main sequence or that it fills the radiative interior as the star evolves on the red giant branch. From these initial conditions, we evolved the magnetic flux, allowing for magnetic diffusion along the evolution of a modeled 1.5 M⊙ star. We find that measured field strengths in red giants attributed to the hydrogen-burning shell are compatible with the field amplitudes and emergence timescales of magnetized white dwarfs. On the contrary, magnetic fields generated solely from a convective-core dynamo on the main sequence and detectable on the red giant branch would be buried too deep in the star and would not match the breakout timescales or the field strengths of magnetic white dwarfs. Therefore, for us to connect magnetic fields observed along the late evolution of stars via a fossil field we would need to find a broadly magnetized internal radiative zone on the red giant branch."}],"language":[{"iso":"eng"}],"oa_version":"Published Version","year":"2026","researchdata_availability":"yes","volume":708,"external_id":{"arxiv":["2601.15203"]},"quality_controlled":"1","citation":{"ieee":"L. Einramhof, L. A. Bugnet, L. M. Calcaferro, L. Barrault, and S. B. Das, “Magneto-archeology of white dwarfs,” <i>Astronomy &#38; Astrophysics</i>, vol. 708. EDP Sciences, 2026.","apa":"Einramhof, L., Bugnet, L. A., Calcaferro, L. M., Barrault, L., &#38; Das, S. B. (2026). Magneto-archeology of white dwarfs. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202659069\">https://doi.org/10.1051/0004-6361/202659069</a>","ama":"Einramhof L, Bugnet LA, Calcaferro LM, Barrault L, Das SB. Magneto-archeology of white dwarfs. <i>Astronomy &#38; Astrophysics</i>. 2026;708. doi:<a href=\"https://doi.org/10.1051/0004-6361/202659069\">10.1051/0004-6361/202659069</a>","ista":"Einramhof L, Bugnet LA, Calcaferro LM, Barrault L, Das SB. 2026. Magneto-archeology of white dwarfs. Astronomy &#38; Astrophysics. 708, L14.","mla":"Einramhof, Lukas, et al. “Magneto-Archeology of White Dwarfs.” <i>Astronomy &#38; Astrophysics</i>, vol. 708, L14, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202659069\">10.1051/0004-6361/202659069</a>.","short":"L. Einramhof, L.A. Bugnet, L.M. Calcaferro, L. Barrault, S.B. Das, Astronomy &#38; Astrophysics 708 (2026).","chicago":"Einramhof, Lukas, Lisa Annabelle Bugnet, L. M. Calcaferro, Lucas Barrault, and S. B. Das. “Magneto-Archeology of White Dwarfs.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202659069\">https://doi.org/10.1051/0004-6361/202659069</a>."},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"doi":"10.1051/0004-6361/202659069","title":"Magneto-archeology of white dwarfs","publication":"Astronomy & Astrophysics","DOAJ_listed":"1","type":"journal_article","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"author":[{"full_name":"Einramhof, Lukas","last_name":"Einramhof","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","first_name":"Lukas"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"},{"full_name":"Calcaferro, L. M.","first_name":"L. M.","last_name":"Calcaferro"},{"full_name":"Barrault, Lucas","first_name":"Lucas","last_name":"Barrault","id":"4471a8fd-32c1-11ee-a9a4-fb670d398f64"},{"first_name":"S. B.","last_name":"Das","full_name":"Das, S. B."}],"article_number":"L14","month":"04","date_created":"2026-08-10T07:53:32Z","day":"01","OA_type":"diamond","fulldoi":"https://doi.org/10.1051/0004-6361/202659069","file_date_updated":"2026-08-11T05:46:02Z","article_type":"original","date_published":"2026-04-01T00:00:00Z","publication_status":"published","scopus_import":"1","das_tickbox":"1","PlanS_conform":"1","OA_place":"publisher"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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.","oa":1,"ddc":["520"],"publisher":"EDP Sciences","has_accepted_license":"1","department":[{"_id":"LiBu"}],"intvolume":"       707","_id":"21659","date_updated":"2026-08-12T09:29:13Z","status":"public","article_processing_charge":"No","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"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"}],"file":[{"file_name":"2026_AstronomyAstrophysics_Breton.pdf","file_size":1535506,"success":1,"date_updated":"2026-04-07T09:20:02Z","date_created":"2026-04-07T09:20:02Z","creator":"dernst","relation":"main_file","access_level":"open_access","checksum":"a7fd798bf450d67d4166fdf54ff2c70c","content_type":"application/pdf","file_id":"21666"}],"oa_version":"Published Version","language":[{"iso":"eng"}],"external_id":{"arxiv":["2603.01979"]},"volume":707,"year":"2026","quality_controlled":"1","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"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).","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>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202659309\">https://doi.org/10.1051/0004-6361/202659309</a>.","ieee":"S. N. Breton <i>et al.</i>, “Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 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.","ama":"Breton SN, Pezzotti C, Mathis S, et al. Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202659309\">10.1051/0004-6361/202659309</a>","apa":"Breton, S. N., Pezzotti, C., Mathis, S., Bugnet, L. A., Di Mauro, M. P., Joergensen, J., … Lanza, A. F. (2026). Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202659309\">https://doi.org/10.1051/0004-6361/202659309</a>","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, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202659309\">10.1051/0004-6361/202659309</a>."},"doi":"10.1051/0004-6361/202659309","title":"Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars","DOAJ_listed":"1","publication":"Astronomy & Astrophysics","type":"journal_article","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"month":"03","article_number":"L16","author":[{"full_name":"Breton, S. N.","first_name":"S. N.","last_name":"Breton"},{"full_name":"Pezzotti, C.","last_name":"Pezzotti","first_name":"C."},{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"},{"first_name":"M. P.","last_name":"Di Mauro","full_name":"Di Mauro, M. P."},{"last_name":"Joergensen","first_name":"J.","full_name":"Joergensen, J."},{"full_name":"Zwintz, K.","first_name":"K.","last_name":"Zwintz"},{"full_name":"Lanza, A. F.","first_name":"A. F.","last_name":"Lanza"}],"date_created":"2026-04-05T22:01:32Z","fulldoi":"https://doi.org/10.1051/0004-6361/202659309","OA_type":"diamond","day":"01","scopus_import":"1","file_date_updated":"2026-04-07T09:20:02Z","article_type":"letter_editor","date_published":"2026-03-01T00:00:00Z","publication_status":"published","OA_place":"publisher","PlanS_conform":"1"},{"intvolume":"       708","department":[{"_id":"LiBu"}],"article_processing_charge":"No","status":"public","date_updated":"2026-10-20T08:14:41Z","_id":"23047","file":[{"creator":"dernst","date_created":"2026-10-07T12:13:55Z","date_updated":"2026-10-07T12:13:55Z","success":1,"file_name":"2026_AstronomyAstrophysics_Leclerc.pdf","file_size":10533299,"content_type":"application/pdf","file_id":"23075","checksum":"868c1be53a4f3e0cf2852a723fcacd08","access_level":"open_access","relation":"main_file"}],"abstract":[{"text":"Aims. We investigate signatures of pressure extrema on global oscillations in discs.\r\n\r\nMethods. We used the framework of wave topology to establish a generalised local dispersion relation that includes pressure gradients. We highlight the influence of a previously unrecognised epicyclic–acoustic frequency, and we derive an analytical criterion for the existence of a branch of modes transiting between the inertial and the pressure bands, known as topological modes.\r\n\r\nResults. We find that pressure extrema consist of wave guides in which such topological modes propagate. The fundamental mode trapped at a pressure bump can propagate at any frequency, allowing it to resonate with any temporal forcing. Conversely, the fundamental mode associated with a pressure dip propagates at any vertical phase velocity. These specific features make them attractive candidates for future discoseismology.","lang":"eng"}],"dataavailabilitystatement":"The scripts written and used for numerical calculations\r\nare accessible at https://github.com/ArmandLeclerc/\r\nradialStratifDisc.","corr_author":"1","project":[{"grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"volume":708,"year":"2026","researchdata_availability":"no","external_id":{"arxiv":["2512.05737"]},"keyword":["accretion","accretion disks","hydrodynamics","instabilities","waves","protoplanetary disks"],"language":[{"iso":"eng"}],"oa_version":"Published Version","oa":1,"ddc":["520"],"acknowledgement":"AL was funded by Contrat Doctoral Spécifique Normaliens during this work. GL, EL and NP acknowledge funding from\r\nERC CoG project PODCAST No 864965. AL acknowledges funding\r\nfrom ERC StG project Calcifer No 101165631. We used Mathematica\r\n(Wolfram Research Inc, 2024).\r\n","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","supplementarymaterial":"yes","publisher":"EDP Sciences","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","date_created":"2026-10-04T22:01:54Z","author":[{"id":"2a1fb1fc-f373-11ef-901a-87cee43a1217","last_name":"Leclerc","first_name":"Armand","full_name":"Leclerc, Armand"},{"full_name":"Laibe, Guillaume","first_name":"Guillaume","last_name":"Laibe"},{"last_name":"Lynch","first_name":"Elliot","full_name":"Lynch, Elliot"},{"full_name":"Perez, Nicolas","first_name":"Nicolas","last_name":"Perez"}],"article_number":"A355","month":"04","publication_status":"published","date_published":"2026-04-01T00:00:00Z","article_type":"original","file_date_updated":"2026-10-07T12:13:55Z","scopus_import":"1","day":"01","OA_type":"diamond","fulldoi":"https://doi.org/10.1051/0004-6361/202558428","PlanS_conform":"1","OA_place":"publisher","das_tickbox":"1","quality_controlled":"1","doi":"10.1051/0004-6361/202558428","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"chicago":"Leclerc, Armand, Guillaume Laibe, Elliot Lynch, and Nicolas Perez. “Radial Modes of Pressure Bumps and Dips in Astrophysical Discs.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202558428\">https://doi.org/10.1051/0004-6361/202558428</a>.","short":"A. Leclerc, G. Laibe, E. Lynch, N. Perez, Astronomy &#38; Astrophysics 708 (2026).","mla":"Leclerc, Armand, et al. “Radial Modes of Pressure Bumps and Dips in Astrophysical Discs.” <i>Astronomy &#38; Astrophysics</i>, vol. 708, A355, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202558428\">10.1051/0004-6361/202558428</a>.","apa":"Leclerc, A., Laibe, G., Lynch, E., &#38; Perez, N. (2026). Radial modes of pressure bumps and dips in astrophysical discs. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202558428\">https://doi.org/10.1051/0004-6361/202558428</a>","ama":"Leclerc A, Laibe G, Lynch E, Perez N. Radial modes of pressure bumps and dips in astrophysical discs. <i>Astronomy &#38; Astrophysics</i>. 2026;708. doi:<a href=\"https://doi.org/10.1051/0004-6361/202558428\">10.1051/0004-6361/202558428</a>","ista":"Leclerc A, Laibe G, Lynch E, Perez N. 2026. Radial modes of pressure bumps and dips in astrophysical discs. Astronomy &#38; Astrophysics. 708, A355.","ieee":"A. Leclerc, G. Laibe, E. Lynch, and N. Perez, “Radial modes of pressure bumps and dips in astrophysical discs,” <i>Astronomy &#38; Astrophysics</i>, vol. 708. EDP Sciences, 2026."},"arxiv":1,"publication":"Astronomy & Astrophysics","DOAJ_listed":"1","title":"Radial modes of pressure bumps and dips in astrophysical discs"},{"quality_controlled":"1","doi":"10.1051/0004-6361/202451541","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"citation":{"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>.","short":"L. Barrault, S. Mathis, L.A. Bugnet, Astronomy &#38; Astrophysics 694 (2025).","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>","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>","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>.","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."},"publication":"Astronomy & Astrophysics","title":"Constraining differential rotation in γ Doradus stars from the properties of inertial dips","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","date_created":"2025-03-02T23:01:53Z","author":[{"first_name":"Lucas","id":"4471a8fd-32c1-11ee-a9a4-fb670d398f64","last_name":"Barrault","full_name":"Barrault, Lucas"},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle"}],"month":"02","article_number":"A225","article_type":"original","publication_status":"published","file_date_updated":"2025-03-04T09:57:03Z","date_published":"2025-02-01T00:00:00Z","scopus_import":"1","day":"01","OA_type":"diamond","fulldoi":"https://doi.org/10.1051/0004-6361/202451541","OA_place":"publisher","ddc":["520"],"oa":1,"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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","has_accepted_license":"1","intvolume":"       694","department":[{"_id":"LiBu"}],"article_processing_charge":"Yes","date_updated":"2026-02-16T12:09:14Z","status":"public","_id":"19283","file":[{"checksum":"568a5e5951f20483663df145a780fc3d","file_id":"19288","content_type":"application/pdf","relation":"main_file","access_level":"open_access","date_created":"2025-03-04T09:57:03Z","date_updated":"2025-03-04T09:57:03Z","creator":"dernst","file_size":7438476,"file_name":"2025_AstronomyAstrophysics_Barrault.pdf","success":1}],"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."}],"corr_author":"1","isi":1,"project":[{"_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631"}],"volume":694,"year":"2025","external_id":{"isi":["001424452400025"]},"language":[{"iso":"eng"}],"oa_version":"Published Version"},{"OA_type":"diamond","day":"01","fulldoi":"https://doi.org/10.1051/0004-6361/202452885","date_published":"2025-09-01T00:00:00Z","file_date_updated":"2025-09-15T06:58:09Z","article_type":"original","publication_status":"published","scopus_import":"1","PlanS_conform":"1","OA_place":"publisher","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","ec_funded":1,"author":[{"full_name":"Vanlaer, V.","last_name":"Vanlaer","first_name":"V."},{"full_name":"Bowman, D. M.","first_name":"D. M.","last_name":"Bowman"},{"first_name":"S.","last_name":"Burssens","full_name":"Burssens, S."},{"orcid":"0000-0003-0896-7972","first_name":"Srijan B","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","last_name":"Das","full_name":"Das, Srijan B"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"full_name":"Aerts, C.","last_name":"Aerts","first_name":"C."}],"month":"09","article_number":"A5","date_created":"2025-09-14T22:01:32Z","citation":{"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.","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>.","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.","ama":"Vanlaer V, Bowman DM, Burssens S, et al. Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452885\">10.1051/0004-6361/202452885</a>","apa":"Vanlaer, V., Bowman, D. M., Burssens, S., Das, S. B., Bugnet, L. A., Mathis, S., &#38; Aerts, C. (2025). Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452885\">https://doi.org/10.1051/0004-6361/202452885</a>","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>."},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"doi":"10.1051/0004-6361/202452885","title":"Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries","publication":"Astronomy & Astrophysics","quality_controlled":"1","project":[{"call_identifier":"H2020","grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"},{"grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"isi":1,"file":[{"checksum":"9ee9f34cf86305602d6cb3e07a1cc1a6","content_type":"application/pdf","file_id":"20354","relation":"main_file","access_level":"open_access","date_updated":"2025-09-15T06:58:09Z","date_created":"2025-09-15T06:58:09Z","creator":"dernst","success":1,"file_size":3175077,"file_name":"2025_AstronomyAstrophysics_Vanlaer.pdf"}],"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."}],"language":[{"iso":"eng"}],"oa_version":"Published Version","volume":701,"year":"2025","external_id":{"arxiv":["2506.19948"],"isi":["001561561200007"]},"department":[{"_id":"LiBu"}],"intvolume":"       701","_id":"20350","article_processing_charge":"No","status":"public","date_updated":"2026-02-16T12:12:53Z","has_accepted_license":"1","publisher":"EDP Sciences","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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"ddc":["520"]},{"fulldoi":"https://doi.org/10.1051/0004-6361/202555213","OA_type":"diamond","day":"01","scopus_import":"1","file_date_updated":"2025-10-13T07:05:55Z","publication_status":"published","date_published":"2025-09-01T00:00:00Z","article_type":"original","OA_place":"publisher","PlanS_conform":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","month":"09","article_number":"A253","author":[{"full_name":"Barrault, Lucas","first_name":"Lucas","last_name":"Barrault","id":"4471a8fd-32c1-11ee-a9a4-fb670d398f64"},{"full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet"},{"last_name":"Mathis","first_name":"S.","full_name":"Mathis, S."},{"full_name":"Mombarg, J. S.G.","last_name":"Mombarg","first_name":"J. S.G."}],"date_created":"2025-10-12T22:01:26Z","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"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>.","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>.","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>","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.","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>"},"doi":"10.1051/0004-6361/202555213","title":"Exploring the probing power of γ Dor's inertial dip for core magnetism: The case of a toroidal field","publication":"Astronomy & Astrophysics","quality_controlled":"1","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"isi":1,"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"}],"corr_author":"1","file":[{"access_level":"open_access","relation":"main_file","content_type":"application/pdf","file_id":"20459","checksum":"2c209b33119af4a251bab4a418a21075","file_size":2503149,"success":1,"file_name":"2025_AstronomyAstrophysics_BarraultL.pdf","creator":"dernst","date_created":"2025-10-13T07:05:55Z","date_updated":"2025-10-13T07:05:55Z"}],"oa_version":"Published Version","language":[{"iso":"eng"}],"external_id":{"arxiv":["2507.00308"],"isi":["001585834500002"]},"year":"2025","volume":701,"department":[{"_id":"LiBu"},{"_id":"GradSch"}],"intvolume":"       701","_id":"20454","date_updated":"2026-02-19T09:32:04Z","status":"public","article_processing_charge":"No","has_accepted_license":"1","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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.","oa":1,"ddc":["520"]},{"DOAJ_listed":"1","publication":"Astronomy & Astrophysics","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields","doi":"10.1051/0004-6361/202557247","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"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>","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>","ista":"Mombarg JSG, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S, Reese DR, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. Astronomy &#38; Astrophysics. 704, A336.","mla":"Mombarg, J. S. G., et al. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A336, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557247\">10.1051/0004-6361/202557247</a>.","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.","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)."},"quality_controlled":"1","OA_place":"publisher","PlanS_conform":"1","scopus_import":"1","date_published":"2025-12-19T00:00:00Z","publication_status":"published","article_type":"original","file_date_updated":"2026-01-05T08:36:28Z","fulldoi":"https://doi.org/10.1051/0004-6361/202557247","day":"19","OA_type":"diamond","date_created":"2026-01-04T23:01:35Z","month":"12","article_number":"A336","author":[{"first_name":"J. S.G.","last_name":"Mombarg","full_name":"Mombarg, J. S.G."},{"full_name":"Vanlaer, V.","first_name":"V.","last_name":"Vanlaer"},{"first_name":"Srijan B","orcid":"0000-0003-0896-7972","last_name":"Das","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","full_name":"Das, Srijan B"},{"full_name":"Rieutord, M.","first_name":"M.","last_name":"Rieutord"},{"last_name":"Aerts","first_name":"C.","full_name":"Aerts, C."},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"},{"first_name":"S.","last_name":"Mathis","full_name":"Mathis, S."},{"first_name":"D. R.","last_name":"Reese","full_name":"Reese, D. R."},{"full_name":"Ballot, J.","first_name":"J.","last_name":"Ballot"}],"ec_funded":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"type":"journal_article","publisher":"EDP Sciences","has_accepted_license":"1","ddc":["520"],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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.","external_id":{"arxiv":["2511.09617"]},"volume":704,"year":"2025","oa_version":"Published Version","language":[{"iso":"eng"}],"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"}],"file":[{"access_level":"open_access","relation":"main_file","file_id":"20937","content_type":"application/pdf","checksum":"d838b4783920c43b7cc866e9cf08b383","file_name":"2025_AstronomyAstrophysics_Mombarg.pdf","file_size":2620909,"success":1,"creator":"dernst","date_updated":"2026-01-05T08:36:28Z","date_created":"2026-01-05T08:36:28Z"}],"project":[{"name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020"},{"grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"date_updated":"2026-07-22T06:20:53Z","status":"public","related_material":{"record":[{"status":"public","relation":"research_data","id":"20936"}]},"article_processing_charge":"No","_id":"20931","intvolume":"       704","department":[{"_id":"LiBu"}]}]