Modeling X-ray Emission From The Coronae Of Low Mass Stars

Details Modeling X-ray Emission From The Coronae Of Low Mass Stars Modeling X-ray Emission From The Coronae Of Low Mass Stars

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21331401g&link_type=abstract

American Astronomical Society, AAS Meeting #213, #314.01; Bulletin of the American Astronomical Society, Vol. 41, p.291

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By extrapolating from observationally derived surface magnetograms of low-mass stars we construct models of their coronal magnetic fields and compare the 3D field geometries 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 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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