The formation of helium lines in the atmospheres of dMe stars

Details The formation of helium lines in the atmospheres of dMe stars The formation of helium lines in the atmospheres of dMe stars

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991iraj...20...84l&link_type=abstract

Irish Astronomical Journal (ISSN 0021-1052), vol. 20, Sept. 1991, p. 84-93.

Physics

3

Chromosphere, Dwarf Stars, Helium, Late Stars, Line Spectra, Stellar Physics, Cosmic X Rays, Heat Balance, Radiative Heat Transfer, Stellar Models

Scientific paper

Chromospheric modeling of late-type stars using hydrogen lines is investigated to calculate corresponding He lines and determine what constraints He puts on the chromosphere. The He lines are compared to observational data to examine the energy balance of the quiescent chromosphere of dMe stars. X-ray heating is considered to be a significant factor in the chromospheres, and the coronal X-rays are required for the effective modeling of the He lines. Because the chromospheric structure is chosen arbitrarily to match the observational constraints, the role of X-rays in the chromospheric heating structure cannot be inferred. It is concluded that coronal backradiation be incorporated into the model and that specific observational data be used to calculate the He lines with more accuracy.

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