Modeling X-ray emission from stellar coronae
Abstract
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.
Cite
@article{arxiv.0809.4222,
title = {Modeling X-ray emission from stellar coronae},
author = {S. G. Gregory and M. Jardine and C. Argiroffi and J. -F. Donati},
journal= {arXiv preprint arXiv:0809.4222},
year = {2009}
}
Comments
4 pages, proceedings of Cool Stars 15, St Andrews, July 2008, to be published in the Conference Proceedings Series of the American Institute of Physics