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Asteroseismology reveals the near-core magnetic field strength in the early-B star HD 43317

Published online by Cambridge University Press:  29 August 2024

D. M. Bowman Open the ORCID record for D. M. Bowman [Opens in a new window] ,
D. Lecoanet  and
T. Van Reeth
D. M. Bowman*
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA
D. Lecoanet
Affiliation:
Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA Department of Engineering Sciences and Applied Mathematics, Northwestern University, Evanston, IL 60208, USA CIERA, Northwestern University, Evanston, IL 60201, USA
T. Van Reeth
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA
*
email: dominic.bowman@kuleuven.be
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Abstract

Spectropolarimetic campaigns have established that large-scale magnetic fields are present at the surfaces of approximately 10% of massive dwarf stars. However, there is a dearth of magnetic field measurements for their deep interiors. Asteroseismology of gravity-mode pulsations combined with rotating magneto-hydrodynamical calculations of the early-B main-sequence star HD 43317 constrain its magnetic field strength to be approximately 5 × 105 G just outside its convective core. This proof-of-concept study for magneto-asteroseismology opens a new window into the observational characterisation of magnetic fields inside massive stars.

Keywords

magnetic fieldsstars: early-typestars: oscillationsstars: rotation
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 218 - 223
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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