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There is growing observational and theoretical evidence suggesting thatatmospheric escape is a key driver of planetary evolution. Commonly, planetaryevolution models employ simple analytic formulae (e.g., energy limited escape)that are often inaccurate, and more detailed physical models of atmosphericloss usually only give snapshots of an atmosphere's structure and are difficultto use for evolutionary studies. To overcome this problem, we upgrade andemploy an already existing upper atmosphere hydrodynamic code to produce alarge grid of about 7000 models covering planets with masses 1 - 39 Earth masswith hydrogen-dominated atmospheres and orbiting late-type stars. The modeledplanets have equilibrium temperatures ranging between 300 and 2000 K. For eachconsidered stellar mass, we account for three different values of thehigh-energy stellar flux (i.e., low, moderate, and high activity). For eachcomputed model, we derive the atmospheric temperature, number density, bulkvelocity, X-ray and EUV (XUV) volume heating rates, and abundance of theconsidered species as a function of distance from the planetary center. Fromthese quantities, we estimate the positions of the maximum dissociation andionisation, the mass-loss rate, and the effective radius of the XUV absorption.We show that our results are in good agreement with previously publishedstudies employing similar codes. We further present an interpolation routinecapable to extract the modelling output parameters for any planet lying withinthe grid boundaries. We use the grid to identify the connection between thesystem parameters and the resulting atmospheric properties. We finally applythe grid and the interpolation routine to estimate atmospheric evolutionarytracks for the close-in, high-density planets CoRoT-7 b and HD219134 b,c...

A grid of upper atmosphere models for 1--40 MEARTH planets: application to CoRoT-7 b and HD219134 b,c