Ultraviolet emission in the MG II H and K lines in Be stars

Details Ultraviolet emission in the MG II H and K lines in Be stars Ultraviolet emission in the MG II H and K lines in Be stars

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...262..675b&link_type=abstract

Astrophysical Journal, Part 1, vol. 262, Nov. 15, 1982, p. 675-681.

Astronomy and Astrophysics

Astrophysics

9

B Stars, Early Stars, Emission Spectra, Metallic Stars, Resonance Lines, Stellar Spectra, Ultraviolet Spectra, Balloon-Borne Instruments, H Lines, K Lines, Lyman Beta Radiation, Magnesium, Stellar Envelopes

Scientific paper

Ultraviolet observations made by the Balloon-borne Ultraviolet Stellar Spectrometer (BUSS) of bright early Be stars reveal emission components to the Mg II doublet at 2800 A. These profiles show central absorption features due to interstellar plus possible circumstellar contributions. These absorption features are bounded by emission lobes on either side. The emission components may in part be due to resonance scattering within the line profile, but there are definite contributions to the emission via a Bowen mechanism driven by Lyman beta. Slight apparent shifts in the absorption components relative to the emission may indicate expansion at approximately 5-10 km/s for the line-forming region giving rise to Mg II. If the material in the shell is accelerated by radiation pressure, comparisons of Mg II velocities with species of higher ionization suggest that the degree of ionization in the shell increases at larger distances from the star. This is not unlike the conditions observed in the stellar winds of O and B supergiants.

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