Radiation Hydrodynamic Models of Eclipsing Low-Mass X-Ray Binaries

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Abstract
We present the results of self-consistent two-dimensional radiation hydrodynamic models of winds and coronae above accretion disks in low-mass X-ray binaries. The numerical method combines adaptive mesh refinement for the hydrodynamics with combined ray tracking/flux-limited diffusion for the radiation. The results of the models are compared with EXOSAT observations of X1822-371 and 2S 0921-630, two eclipsing systems that are ideal for direct tests of coronal structure. Excellent fits to the eclipses by the companion star are found for models with intrinsic system luminosities ≈ 0.1LEdd. Estimates are made of the equivalent width of the Fe Kα emission, and values in the range 50-200 eV are found, comparable to estimates from recent observations.

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