The intrinsic LY α to H α ratio in M dwarf stars.

Details The intrinsic LY α to H α ratio in M dwarf stars. The intrinsic LY α to H α ratio in M dwarf stars.

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...318..835d&link_type=abstract

Astronomy and Astrophysics, v.318, p.835-840

Astronomy and Astrophysics

Astrophysics

6

Lines: Profiles, Stars: Activity: Chromospheres, Late-Type, Ism: General

Scientific paper

Using Ly α line profiles generated from a grid of M dwarf model atmospheres we calculate the attenuation factor [i.e. Lyα(obs)/Lyα(intrin)] due to the interstellar medium as a function of hydrogen column density. Then using selected model atmospheres, attenuation factors were calculated for those M dwarfs with available Ly α observations. The prime motivation in this work has been to look afresh at the intrinsic Ly α to H α flux ratio, an important constraint in the radiative transfer modelling of M dwarfs. For those active dMe stars where both lines were observed, the intrinsic ratio is ~3-5 (with ~50% variation). The major uncertainty in this work has been the interstellar hydrogen column density, emphasizing the need for further work in this area and in particular an accurate model of its variation in all directions.

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