Hydrogen non-LTE computations in M dwarf chromospheres

Details Hydrogen non-LTE computations in M dwarf chromospheres Hydrogen non-LTE computations in M dwarf chromospheres

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992iraj...20..197p&link_type=abstract

(Astronomical Science Group of Ireland, Meeting, Regional Technical College, Cork, Republic of Ireland, Sept. 14, 1990) Irish As

Statistics

Computation

Chromosphere, Dwarf Stars, H Alpha Line, M Stars, Nonequilibrium Thermodynamics, Stellar Atmospheres, Electron Density (Concentration), Lyman Alpha Radiation, Stellar Activity

Scientific paper

Analytical techniques are described for calculating the hydrogen lines of the chromospheres of M dwarf stars with details given of the atomic model used for the non-LTE computations. The model is made up of nine bound levels plus continuum and addresses all radiative and collisional transitions between the first eight levels. A substantial increase in electron density is noted for small increases in the transition-region temperature gradient of the stars. The calculations yield important information regarding the Balmer series and the effects of surface gravity on the Balmer profiles.

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