Temperature and density dependence of the Lyman alpha line wing in hydrogen-rich white dwarf atmospheres

Details Temperature and density dependence of the Lyman alpha line wing in hydrogen-rich white dwarf atmospheres Temperature and density dependence of the Lyman alpha line wing in hydrogen-rich white dwarf atmospheres

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...242..133a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 242, no. 1, Feb. 1991, p. 133-141. DOE-supported research.

Astronomy and Astrophysics

Astrophysics

18

Line Spectra, Lyman Alpha Radiation, Stellar Atmospheres, White Dwarf Stars, Absorption Spectra, Hydrogen Atoms, Temperature Dependence, Ultraviolet Spectra

Scientific paper

A new calculation of resonance broadening in the far wing of Ly-alpha that is applicable to DA white dwarfs is presented. This analysis invokes an expansion in powers of the atomic hydrogen density, and uses accurate potentials for two states of H2 to provide realistic estimates of extreme far wing profiles for the first time. Absorption during the close collision with one or more atoms or ions is probable, and produces significant effects throughout the line wing. New satellites are predicted near 1900 and 2400 A due to three-body H3(+) and H3 interactions. Such effects are identified in some IUE white dwarf spectra. At densities above 10 to the 21st/cu cm all of the transition probability for Ly-alpha is shown to occur in its far wing, influencing even the visible region above 4000 A.

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