Abstract

Using general stellar atmosphere code PHOENIX, the influence of chemi‐ionization and inverse chemi‐recombination processes, in H*(n)+H(1s) collisions, on the population of higher levels and consequently on profiles of Hydrogen lines in the atmospheres of late type (M) stars was studied. Obtained results are the first demonstration of the possibility to confirm the considered processes influence by direct observations of stellar spectra. It is demonstrated that it is very important to include chemi‐ionization and chemi‐recombination processes in modeling of atmospheres of late type stars, especially if one wants to use line profiles for diagnostics of stellar photospheres and lower chromospheres.

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