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Interior rotation modelling of the β Cep pulsator HD 192575 including multiplet asymmetries

Lookup NU author(s): Dr Dominic BowmanORCiD

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This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).

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.

Publication metadata

Author(s): Vanlaer V, Bowman DM, Burssens S, Bharati Das S, Bugnet L, Mathis S, Aerts C

Publication type: Article

Publication status: Published

Journal: Astronomy & Astrophysics

Year: 2025

Volume: 701

Pages: 13

Print publication date: 01/09/2025

Online publication date: 01/09/2025

Acceptance date: 09/07/2025

Date deposited: 07/05/2026

ISSN (print): 0004-6361

ISSN (electronic): 1432-0746

Publisher: EDP Sciences

URL: https://doi.org/10.1051/0004-6361/202452885

DOI: 10.1051/0004-6361/202452885

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Funding

Funder referenceFunder name
European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N◦101165631)
Frontier Research grant under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1)
European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No 101034413
Horizon Europe programme (Synergy Grant agreement N◦101071505: 4D-STAR
Research Foundation Flanders (FWO) under grant K802922N (Sabbatical leave)
Research Foundation Flanders (FWO; grant number: 1286521N)
Royal Society University Research Fellowship (URF; grant number: URF\R1\231631)
PLATO CNES grant at CEA/DAp
w 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).

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