Hydrogen infrared recombination line profiles in Be star winds

Details Hydrogen infrared recombination line profiles in Be star winds Hydrogen infrared recombination line profiles in Be star winds

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...253l..25w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 253, no. 2, Jan. 1992, p. L25-L28. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

20

B Stars, Hydrogen Recombinations, Infrared Spectra, Spectral Line Width, Stellar Winds, Radial Velocity, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

Theoretical hydrogen infrared recombination line profiles from flattened rotating and slowly expanding disks around Be stars are presented. The IR lines show a double-peaked structure characteristic of rotating disks, but with a V/R ratio which is reversed compared to the V/R ratio of the H-alpha line. This effect can be explained in terms of the formation region of the lines in combination with continuum optical depth effects that affect the IR lines. The calculations demonstrate that some emission lines from rotating and expanding disks can also show a violet peak that is stronger than the red peak (V greater than R). Infrared recombination line profiles are sensitive probes of the velocity and density structure of their region of formation.

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