Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (147) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (26)
· Also-Read Articles (Reads History)
·
· Translate This Page
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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints
    


SAO/NASA ADS Homepage | ADS Sitemap | Query Form | Basic Search | Preferences | HELP | FAQ