Hostname: page-component-5c6d5d7d68-wtssw Total loading time: 0 Render date: 2024-08-29T16:36:57.688Z Has data issue: false hasContentIssue false
  • English
  • Français

Can we detect deep axisymmetric toroidal magnetic fields in stars?

Published online by Cambridge University Press:  29 August 2024

Hachem Dhouib Open the ORCID record for Hachem Dhouib [Opens in a new window] ,
Stéphane Mathis ,
Lisa Bugnet ,
Timothy Van Reeth  and
Conny Aerts
Hachem Dhouib*
Affiliation:
Université Paris Cité, Université Paris-Saclay, CEA, CNRS, Astrophysique, Instrumentation et Modélisation Paris-Saclay, F-91191, Gif-sur-Yvette, France
Stéphane Mathis
Affiliation:
Université Paris Cité, Université Paris-Saclay, CEA, CNRS, Astrophysique, Instrumentation et Modélisation Paris-Saclay, F-91191, Gif-sur-Yvette, France
Lisa Bugnet
Affiliation:
Flatiron Institute, Simons Foundation, 162 Fifth Ave, New York, NY 10010, USA
Timothy Van Reeth
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
Conny Aerts
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, the Netherlands Max Planck Institute for Astronomy, Koenigstuhl 17, 69117 Heidelberg, Germany
*
email: hachem.dhouib@cea.fr
Get access Rights & Permissions [Opens in a new window]

Abstract

The current angular momentum (AM) transport models fail to reproduce asterosieimic observations. One of the best candidates to explain this discrepancy is the magnetic field in radiative zones with its various possible topologies, for instance axisymmetric toroidal magnetic field. If such azimuthal field is strong enough, the Tayler’s instability could occur which induces a magnetic torque that allows a very efficient transport of AM and could trigger dynamo action in radiative layers. If such important field does not emerge at the surface, spectropolarimetry is blind. In this case, the only way to detect and characterise the field is by using magneto-asteroseismology. It consists in searching for the characteristic signatures of magnetic field in the observed frequency spectra of stellar oscillations.

Keywords

stars: early-typestars: interiorsstars: magnetic fields
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 238 - 240
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Dhouib, H., Mathis, S., Bugnet, L., Van Reeth, T., & Aerts, C. 2022, A&A, 661, A133 CrossRefGoogle Scholar
Fuller, J., Piro, A. L., & Jermyn, A. S. 2019, MNRAS, 485, 3661 Google Scholar
Laplace, P. S. 1799, Traité de Mécanique Cëleste (Imprimerie de Crapelet (Paris))Google Scholar
Lee, U. & Saio, H. 1997, ApJ, 491, 839 CrossRefGoogle Scholar
Mathis, S., Bugnet, L., Prat, V., et al. 2021, A&A, 647, A122 Google Scholar
Neiner, C., Mathis, S., Alecian, E., et al. 2015, in Polarimetry, ed. Nagendra, K. N., Bagnulo, S., Centeno, R., & Jesús Martnez, M. González, Vol. 305, 61–66 Google Scholar
Spruit, H. C. 2002, A&A, 381, 923 Google Scholar
Zahn, J. P., Brun, A. S., & Mathis, S. 2007, A&A, 474, 145 CrossRefGoogle Scholar
Supplementary material: PDF

Dhouib et al. supplementary material

Dhouib et al. supplementary material

Download Dhouib et al. supplementary material(PDF)
PDF 1.8 MB