Modeling X-ray emission from stellar coronae

Details Modeling X-ray emission from stellar coronae Modeling X-ray emission from stellar coronae

2008-09-24

arxiv.org/abs/0809.4222v1

Astronomy and Astrophysics

Astrophysics

4 pages, proceedings of Cool Stars 15, St Andrews, July 2008, to be published in the Conference Proceedings Series of the Amer

Scientific paper

10.1063/1.3099184

By extrapolating from observationally derived surface magnetograms 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.

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