Acoustic and magnetic wave heating in stars - III. The chromospheric emission-magnetic filling factor relation

被引：26
作者：
Fawzy, D
Stepien, K
Ulmschneider, P
Rammacher, W
Musielak, ZE
机构：
[1] Univ Heidelberg, Inst Theoret Astrophys, D-69121 Heidelberg, Germany
[2] Univ Warsaw Observ, PL-00478 Warsaw, Poland
[3] Univ Texas, Dept Phys, Arlington, TX 76019 USA
来源：
ASTRONOMY & ASTROPHYSICS | 2002年 / 386卷 / 03期
关键词：
methods : numerical; stars : chromospheres; stars : coronae; stars : magnetic fields; MHD; waves;
D O I：
10.1051/0004-6361:20020253
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Theoretical chromospheric models described in the two previous papers of this series are used to study the relationship between the chromospheric emission and the filling factor. This theoretically determined relationship shows that the chromospheric emission flux in Ca II (H+K) is approximately proportional to the square root of the magnetic filling factor at the stellar surface. To relate the filling factor to stellar rotation rate, we compare the theoretical fluxes with observations of stars with known rotation period. The comparison shows that the Rossby number is probably a more appropriate measure of the rotation influence on activity of main-sequence stars than the rotation period. Our theoretical Mg II (h+k) and Ca II (H+K) emission fluxes are also found to be well correlated, which is in a good agreement with the observational data.
引用
收藏
页码：994 / 1000
页数：7
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