Volume 541, May 2012
|Number of page(s)||4|
|Published online||03 May 2012|
Inelastic Mg+H collision data for non-LTE applications in stellar atmospheres
Department of Physics and AstronomyUppsala University,
2 Department of Theoretical Physics, Herzen University, St. Petersburg 191186, Russia
3 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching bei München, Germany
4 LERMA, Observatoire de Paris, 92195 Meudon Cedex, France
5 Université Paris-Est, Laboratoire Modélisation et Simulation Multi-Echelle, MSME UMR 8208 CNRS, 5 Bd Descartes, 77454 Marne-la-Vallée, France
Received: 21 February 2012
Accepted: 21 March 2012
Rate coefficients for inelastic Mg+H collisions are calculated for all transitions between the lowest seven levels and the ionic state (charge transfer), namely Mg(3s2 1S, 3s3p 3P, 3s3p 1P, 3s4s 3S, 3s4s 1S, 3s3d 1D, 3s4p 3P)+H(1s) and Mg+(3s 2S)+H−. The rate coefficients are based on cross-sections from full quantum scattering calculations, which are themselves based on detailed quantum chemical calculations for the MgH molecule. The data are needed for non-LTE applications in cool astrophysical environments, especially cool stellar atmospheres, and are presented for a temperature range of 500−8000 K. From consideration of the sensitivity of the cross-sections to various uncertainties in the calculations, most importantly input quantum chemical data and the numerical accuracy of the scattering calculations, a measure of the possible uncertainties in the rate coefficients is estimated.
Key words: atomic data / line: formation / stars: abundances
© ESO, 2012
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