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Title:
Atomic and molecular line emission from early-type high-luminosity stars
Authors:
McGregor, P. J.; Hyland, A. R.; Hillier, D. J.
Affiliation:
AA(Mount Stromlo and Siding Spring Observatories, Canberra, Australia), AB(Mount Stromlo and Siding Spring Observatories, Canberra, Australia), AC(Anglo-Australian Observatory, Epping, Australia)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 15, 1988, p. 1071-1098. (ApJ Homepage)
Publication Date:
01/1988
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ATOMIC SPECTRA, EARLY STARS, EMISSION SPECTRA, INFRARED SPECTROSCOPY, MOLECULAR SPECTRA, STELLAR MASS EJECTION, STELLAR SPECTRA, CARBON MONOXIDE, INFRARED ASTRONOMY, STELLAR WINDS
DOI:
10.1086/165964
Bibliographic Code:
1988ApJ...324.1071M

Abstract

An infrared spectroscopic investigation (1.0 - 2.5 μm) of high-luminosity early-type emission line stars has been carried out. Emission lines of H I and He I dominate the near-infrared spectra, while emission lines of [Fe II], Mg II, Na I, and Fe II are also seen in some objects. The authors derive mass-loss rates from Brγ fluxes ranging from 3×10-7M_sun;yr-1 for the B supergiant HR Car to more than 3×10-5M_sun;yr-1 for the extreme P Cygni star HD 316285. A subset of the stars shows the first-overtone band heads of CO in emission. The presence of molecular CO in the extended envelopes is difficult to reconcile with the large ultraviolet fluxes from these stars and suggests that the CO emitting material lies at a radius of ≡1016cm and is either swept-up remnant material lost from the star in a cool stellar wind when the star was a red supergiant or is material located in a cool disk around the star.

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