Theoretical P Cygni profiles for resonance lines from excited levels

Details Theoretical P Cygni profiles for resonance lines from excited levels Theoretical P Cygni profiles for resonance lines from excited levels

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245.1054o&link_type=abstract

Astrophysical Journal, Part 1, vol. 245, May 1, 1981, p. 1054-1059.

Astronomy and Astrophysics

Astronomy

24

Resonance Lines, Stellar Mass Ejection, Stellar Spectra, Stellar Spectrophotometry, Ultraviolet Astronomy, Digital Techniques, Iue, Line Spectra, Population Theory, Radial Velocity, Stellar Winds, Ultraviolet Spectra, Wolf-Rayet Stars

Scientific paper

In stars with very dense expanding winds (for example, Of and Wolf-Rayet stars), the populations of the excited levels of ions can easily be large enough to produce observable line profiles of the P Cygni type. Since the populations of the lower levels of the observed transitions have strong dependences upon the radial distance from the star, previously published resonance line profiles are not adequate for fitting lines from excited levels. An atlas of appropriate profiles is presented and the procedure for determining mass loss rates is discussed.

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