Hostname: page-component-745bb68f8f-b6zl4 Total loading time: 0 Render date: 2025-01-12T21:13:05.903Z Has data issue: false hasContentIssue false
  • English
  • Français

Combining magnetic and seismic studies to constrain processes in massive stars

Published online by Cambridge University Press:  07 August 2014

Coralie Neiner ,
Pieter Degroote ,
Blanche Coste ,
Maryline Briquet  and
Stéphane Mathis
Coralie Neiner
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France email: [email protected]
Pieter Degroote
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France email: [email protected] Instituut voor Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium
Blanche Coste
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France email: [email protected]
Maryline Briquet
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Bât B5c, 4000 Liège, Belgium
Stéphane Mathis
Affiliation:
LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Univ. Paris Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France email: [email protected] Laboratoire AIM Paris-Saclay, CEA/DSM-CNRS-Université Paris Diderot; IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The presence of pulsations influences the local parameters at the surface of massive stars and thus it modifies the Zeeman magnetic signatures. Therefore it makes the characterisation of a magnetic field in pulsating stars more difficult and the characterisation of pulsations is thus required for the study of magnetic massive stars. Conversely, the presence of a magnetic field can inhibit differential rotation and mixing in massive stars and thus provides important constraints for seismic modelling based on pulsation studies. As a consequence, it is necessary to combine spectropolarimetric and seismic studies for all massive classical pulsators. Below we show examples of such combined studies and the interplay between physical processes.

Keywords

stars: early-typestars: magnetic fieldsstars: oscillations (including pulsations)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 302 - 303
Copyright
Copyright © International Astronomical Union 2014 

References

Briquet, M., Neiner, C., Aerts, C.et al. 2012, MNRAS, 427, 483Google Scholar
Briquet, M., Neiner, C., Leroy, B.et al. 2013, A&A, 557L, 16Google Scholar
Mathis, S. & Zahn, J.-P. 2005, A&A, 440, 653Google Scholar
Neiner, C., Alecian, E., Briquet, M.et al. 2012, A&A, 537A, 148Google Scholar
Papics, P., Briquet, M., Baglin, A.et al. 2012, A&A, 542A, 55Google Scholar
Shibahashi, H. & Aerts, C. 2000, ApJ, 531L, 143CrossRefGoogle Scholar
Spruit, H. 1999, A&A, 349, 189Google Scholar
Zahn, J.-P. 2011, IAUS, 272, 14Google Scholar