Emission-line spectra of circumstellar envelopes - Infrared hydrogen line fluxes from Be stars

Details Emission-line spectra of circumstellar envelopes - Infrared hydrogen line fluxes from Be stars Emission-line spectra of circumstellar envelopes - Infrared hydrogen line fluxes from Be stars

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aj.....90.1860p&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 90, Sept. 1985, p. 1860-1869. NSF-supported research.

Astronomy and Astrophysics

Astronomy

20

B Stars, Emission Spectra, Hydrogen, Infrared Astronomy, Stellar Envelopes, Stellar Spectra, Continuous Spectra, Spectral Line Width, Stellar Mass Ejection, Visible Spectrum

Scientific paper

Fluxes for eight H I emission lines between 1.28 and 4.67 μm are presented for a sample of seven Be stars. Brα fluxes are given for six additional Be stars. The H I line ratios form the basis for an observational test of models for emission from circumstellar shells that have a range of Brα optical depths well in excess of unity. Enough data on optically thick H I, Ca II, and O I line strengths of circumstellar envelope stars now exist that it should be possible to place detailed radiative-transfer calculations of optically thick envelope emission on a secure observational footing. Comparisons of line ratios with the models by Simon et al. for infrared line emission from stellar winds show promise. The Be star H I line ratios can also be compared with similar data for deeply dust-embedded young stellar objects. These enigmatic objects display stronger H I lines per unit luminosity than the Be stars, but share similar overall envelope physical conditions. Several infrared line ratios are examined to lay the groundwork for extinction determinations and guidelines for radiative-transfer models.

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