Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries
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 and Astrophysics. 701, A5.
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Author
Vanlaer, V.;
Bowman, D. M.;
Burssens, S.;
Das, Srijan BISTA 
;
Bugnet, LisaISTA ;
Mathis, S.;
Aerts, C.
;
Bugnet, LisaISTA ;
Mathis, S.;
Aerts, C.Department
Grant
Abstract
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.
Aims. 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.
Methods. 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.
Results. 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.
Conclusions. 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.
Publishing Year
Date Published
2025-09-01
Journal Title
Astronomy and Astrophysics
Publisher
EDP Sciences
Acknowledgement
The authors appreciated the critical comments from the
referee, which encouraged V.V. to embark upon a new code development
sprint. V.V. gratefully acknowledges support from the Research Foundation
Flanders (FWO) under grant agreement N◦1156923N (PhD Fellowship) and
N
◦K233724N (Travel grant). D.M.B. gratefully acknowledges support from
the Research Foundation Flanders (FWO; grant number: 1286521N), and UK
Research and Innovation (UKRI) in the form of a Frontier Research grant under
the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY;
grant number: EP/Y031059/1), and a Royal Society University Research Fellowship (URF; grant number: URF\R1\231631). S.B.D. acknowledges funding from
the European Union’s Horizon 2020 research and innovation programme under
the Marie Skłodowska-Curie grant agreement No 101034413. L.B. gratefully
acknowledges support from the European Research Council (ERC) under the
Horizon Europe programme (Calcifer; Starting Grant agreement N◦101165631).
S.M. acknowledges support from the PLATO CNES grant at CEA/DAp.C.A.
acknowledges financial support from the Research Foundation Flanders (FWO)
under grant K802922N (Sabbatical leave); she is grateful for the kind hospitality
offered by CEA/Saclay during her sabbatical work visits in the spring of 2023.
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 funded by the European Union,
views and opinions expressed are however those of the author(s) 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 TESS data presented in this paper were obtained from
the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Support to
MAST for these data is provided by the NASA Office of Space Science via grant
NAG5-7584 and by other grants and contracts. Funding for the TESS mission
was provided by the NASA Explorer Program.
Volume
701
Article Number
A5
ISSN
eISSN
IST-REx-ID
Cite this
Vanlaer V, Bowman DM, Burssens S, et al. Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. Astronomy and Astrophysics. 2025;701. doi:10.1051/0004-6361/202452885
Vanlaer, V., Bowman, D. M., Burssens, S., Das, S. B., Bugnet, L. A., Mathis, S., & Aerts, C. (2025). Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries. Astronomy and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452885
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.” Astronomy and Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452885.
V. Vanlaer et al., “Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries,” Astronomy and Astrophysics, vol. 701. EDP Sciences, 2025.
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 and Astrophysics. 701, A5.
Vanlaer, V., et al. “Interior Rotation Modelling of the β Cep Pulsator HD 192575 Including Multiplet Asymmetries.” Astronomy and Astrophysics, vol. 701, A5, EDP Sciences, 2025, doi:10.1051/0004-6361/202452885.
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