Replication data for: Simulating the X-ray emission from accretion shocks on T Tauri stars

Classical T Tauri stars (CTTS) are surrounded by actively accreting disks. According to current models material falls along the magnetic field lines from the disk with more or less free-fall velocity onto the star, where the plasma heats up and generates X-rays. We want to quantitatively explain the observed high energy emission and measure the infall parameters from the data. Absolute flux measurements allow to calculate the filling factor and the mass accretion rate. We use a numerical model of the hot accretion spot and solve the conservation equations, taking into account explicitly non-equilibrium ionisation states in a two-fluid approximation. This study provides (1) a fits file that contains a model grid. The format of the fits file allows to easily use it a a table model for fitting accretion spots in the common X-ray data fitting programs XSPEC and Sherpa. (2) There are the hydrodynamical information (e.g. temperature and density profiles) for a grid of models. Details of the model can be found in the two publications given uder "Publications".