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CP and related phenomena in the context of Stellar Evolution

Published online by Cambridge University Press:  21 October 2010

J. Braithwaite ,
T. Akgün ,
E. Alecian ,
A. F. Kholtygin ,
J. D. Landstreet ,
S. Mathis ,
G. Michaud ,
J. Portnoy ,
G. Alecian  and
V. D. Bychkov
...Show all authors
J. Braithwaite
Affiliation:
Canadian Institute for Theoretical Astrophysics, Toronto, Canada Argelander Institut für Astronomie, Bonn, Germany; [email protected]
T. Akgün
Affiliation:
Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; [email protected]
E. Alecian
Affiliation:
Observatoire de Paris, LESIA, 5 place Jules Janssen, 92190 Meudon, [email protected]
A. F. Kholtygin
Affiliation:
Department of Astronomy, Saint-Petersburg State University, Saint-Petersburg, Russia; [email protected]
J. D. Landstreet
Affiliation:
University of Western Ontario, 1151 Richmond Street, London ON N6A 3K7, Canada Armagh Observatory, Northern Ireland
S. Mathis
Affiliation:
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191 Gif-sur-Yvette, France; [email protected]
G. Michaud
Affiliation:
Département de Physique, Université de Montréal, Montréal, PQ, H3C 3J7, Canada; [email protected]
J. Portnoy
Affiliation:
Sami Shamoon College of Engineering, [email protected]
G. Alecian
Affiliation:
Observatoire de Paris, LESIA, 5 place Jules Janssen, 92190 Meudon, [email protected]
V. D. Bychkov
Affiliation:
Special Astrophysical Observatory, Russia
L. V. Bychkova
Affiliation:
Special Astrophysical Observatory, Russia
N. Drake
Affiliation:
Department of Astronomy, Saint-Petersburg State University, Saint-Petersburg, Russia; [email protected]
S. N. Fabrika
Affiliation:
Special Astrophysical Observatory, Russia
A. Reisenegger
Affiliation:
Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; [email protected]
R. Steinitz
Affiliation:
Physics Dept., Ben Gurion University of the Negev, Israel
M. Vick
Affiliation:
Département de Physique, Université de Montréal, Montréal, PQ, H3C 3J7, Canada; [email protected]
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Abstract

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We review the interaction in intermediate and high mass stars between their evolution and magnetic and chemical properties. We describe the theory of Ap-star ‘fossil’ fields, before touching on the expected secular diffusive processes which give rise to evolution of the field. We then present recent results from a spectropolarimetric survey of Herbig Ae/Be stars, showing that magnetic fields of the kind seen on the main-sequence already exist during the pre-main sequence phase, in agreement with fossil field theory, and that the origin of the slow rotation of Ap/Bp stars also lies early in the pre-main sequence evolution; we also present results confirming a lack of stars with fields below a few hundred gauss. We then seek which macroscopic motions compete with atomic diffusion in determining the surface abundances of AmFm stars. While turbulent transport and mass loss, in competition with atomic diffusion, are both able to explain observed surface abundances, the interior abundance distribution is different enough to potentially lead to a test using asterosismology. Finally we review progress on the turbulence-driving and mixing processes in stellar radiative zones.

Keywords

stars: magnetic fields – stars: chemically peculiar – stars: evolution – (magnetohydrodynamics) MHD – stars: rotation – stars: intermediate mass – stars: pre-main sequence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 161 - 171
Copyright
Copyright © International Astronomical Union 2010

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