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arXiv 1002.4091astro-ph.SR
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恒星演化背景下的CP和相关现象

CP and related phenomena in the context of Stellar Evolution

J. Braithwaite, T. Akgün, E. Alecian, A. F. Kholtygin, J. D. Landstreet, S. Mathis, G. Michaud, J. Portnoy, G. Alecian, V. D. Bychkov, L. V. Bychkova, N. Drake,… 展开作者

J. Braithwaite, T. Akgün, E. Alecian, A. F. Kholtygin, J. D. Landstreet, S. Mathis, G. Michaud, J. Portnoy, G. Alecian, V. D. Bychkov, L. V. Bychkova, N. Drake, S. N. Fabrika, A. Reisenegger, R. Steinitz, M. Vick

备注：
Proceedings of IAU GA in Rio, JD4 on Ap stars; 10 pages, 7 figures
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摘要：

本文综述了中、高质量恒星的演化与其磁性和化学性质之间的相互作用。我们描述了理论的AP-星“化石”领域，在触及预期的长期扩散过程，从而引起该领域的演变。然后，我们介绍了Herbig Ae/Be星的光谱偏振测量的最新结果，表明主序上看到的那种磁场在主序前阶段已经存在，与化石场论一致，并且Ap/Bp星缓慢旋转的起源也位于主序前演化的早期;我们还提出了结果，确认缺乏恒星的领域低于几百高斯。然后，我们寻求哪些宏观运动与原子扩散竞争，以确定表面丰度的AmFm星。虽然湍流运输和质量损失，在竞争原子扩散，都能够解释观测到的表面丰度，内部丰度分布是不同的，足以潜在地导致使用asterosismology测试。最后，我们回顾了恒星辐射带中的相干驱动和混合过程的研究进展。

英文摘要：

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.

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