Influence of chemi-ionization and chemi-recombination processes on hydrogen line shapes in M dwarfs

被引：14
作者：
Mihajlov, A. A.
Jevremovic, D.
Hauschildt, P.
Dimitrijevic, M. S.
Ignjatovic, Lj. M.
Alard, F.
机构：
[1] Inst Phys, Belgrade 11001, Serbia
[2] Astron Observ, Belgrade 11160, Serbia
[3] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA
[4] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA
[5] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany
[6] ENS, CRAL, F-69634 Lyon 07, France
来源：
ASTRONOMY & ASTROPHYSICS | 2007年 / 471卷 / 02期
关键词：
atomic processes; molecular processes; stars : atmosphere; line : formation; stars : chromospheres; stars : late-type;
D O I：
10.1051/0004-6361:20077517
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Aims. We study the influence of chemi-ionization in H*(n) + H(1s) collisions and inverse chemi-recombination processes on the population of higher levels and consequently on profiles of hydrogen lines in the atmospheres of late type ( M) stars. Methods. Modeling, using general stellar atmosphere code PHOENIX to reveal the importance of the inclusion of such processes. Results. We demonstrate for the first time observationally detectable effects of these chemi-processes on stellar spectra. Conclusions. It is very important to include chemi-ionization and chemi-recombination processes in modeling of atmospheres of late type stars, especially if one wants to use line profiles for diagnostics of stellar photospheres and lower chromospheres.
引用
收藏
页码：671 / 673
页数：3
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