Modeling X-ray emission from stellar coronae

被引：0

作者：

Gregory, S. G. ^{[1
]}

Jardin, M. ^{[1
]}

Argiroffi, C. ^{[2
,3
]}

Donati, J. -F. ^{[4
]}

机构：

[1] Univ St Andrews, Dept Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland

[2] Univ Palermo, Dipartimento Sci Fis Astron, I-90134 Palermo, Italy

[3] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy

[4] Univ Toulouse, CNRS, LATT, F-31400 Toulouse, France

来源：

COOL STARS, STELLAR SYSTEMS AND THE SUN | 2009年 / 1094卷

关键词：

Stars: coronae; Stars: activity; Xrays: stars; Stars: individual: AB Dor; V374; Peg; FULLY CONVECTIVE STAR; T-TAURI STARS; AB-DORADUS; DIFFERENTIAL ROTATION; MAGNETIC TOPOLOGY;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

By extrapolating from observationally derived surface magneto-rams of low-mass stars we Construct models of their coronal magnetic fields and compare the 3D field geometry with axial multipoles. AB Dor, which has a radiative core. has a very complex field, whereas V374 Peg, which is completely convective. has a simple dipolar field. We calculate global X-ray emission measures assuming that the plasma trapped along the coronal loops is in hydrostatic equilibrium and compare the differences between;assuming isothermal coronae, or by considering a loop temperature profiles. Our preliminary results suggest that the non-isothermal model works well for the complex field of AB Dor, but not for the simple field of V374 Peg.

引用

页码：600 / +

页数：2

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