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1989•International Astronomical Union ColloquiumOpen access

Chromospheric NLTE-Radiative-Transfer Modeling of dMe Stars

P. M. Panagi, E. R. Houdebine, C. John Butler, Marcello Rodono

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Abstract

Abstract The formation of the Lyman and Balmer lines of Hydrogen at densities typical in dMe stars is shown to be very dependent on the atomic model used viz. the number of levels and line transitions. The effect of increasing the number of levels and line transitions on the line fluxes and ionization fraction is also discussed.

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Abstract The formation of the Lyman and Balmer lines of Hydrogen at densities typical in dMe stars is shown to be very dependent on the atomic model used viz. the number of levels and line transitions. The effect of increasing the number of levels and line transitions on the line fluxes and ionization fraction is also discussed.

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Available abstract

Abstract The formation of the Lyman and Balmer lines of Hydrogen at densities typical in dMe stars is shown to be very dependent on the atomic model used viz. the number of levels and line transitions. The effect of increasing the number of levels and line transitions on the line fluxes and ionization fraction is also discussed.

Key concepts: Balmer series, Radiative transfer, Stars, Physics, Ionization, Astrophysics, Line (geometry), Hydrogen

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