The boundary between the magnetic fields of ap stars and the fields of solar-type stars
The boundary between the magnetic fields of ap stars and the fields of solar-type stars
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ap星的磁场与太阳型恒星的磁场之间的边界
DOI：
10.1007/3-540-53955-7_153
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发表时间：
1991
影响因子：
6.9
通讯作者：
J. Landstreet
中科院分区：
文献类型：
--
作者：
J. Landstreet
太阳型星的磁场和太阳型星的磁场之间的边界出现在Te = 7000K附近，这是主序星中深包层对流发展的地方。这对于太阳型恒星来说似乎是很自然的，因为磁场是由对流区产生的。然而，在磁性Ap星中，出现的频率从A0附近所有A星的10%下降到F0附近的1%。目前还不清楚是什么导致了频率的下降，但对流区可能不是原因。事实上，如果在主序星F中出现全球化石场，那么即使这些恒星的化学性质并不特殊，也应该可以探测到这样的场。
The boundary between Ap-type magnetic fields and the magnetic fields of solar-type stars occurs near Te ∼ 7000K, about where deep envelope convection develops in main sequence stars. This seems natural for solar-type stars, in which the field is generated by the convection zone. However, among magnetic Ap stars the frequency of occurrence declines from about 10% of all A stars near A0 to about 1% near F0. It is not clear what produces this decline in frequency, but the convection zone is probably not responsible. In fact, it seems likely that if global fossil fields occur in main sequence F stars, such fields should be detectable even if the stars having them are not chemically peculiar.