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)
· References in the article
· Citations to the Article (1373) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Radiation-driven winds in Of stars
Authors:
Castor, J. I.; Abbott, D. C.; Klein, R. I.
Affiliation:
AA(Joint Institute for Laboratory Astrophysics; Colorado, University, Boulder, Colo.), AB(Joint Institute for Laboratory Astrophysics, Boulder, Colo.), AC(Joint Institute for Laboratory Astrophysics, Boulder, Colo.)
Publication:
Astrophysical Journal, vol. 195, Jan. 1, 1975, pt. 1, p. 157-174. (ApJ Homepage)
Publication Date:
01/1975
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Astronomical Models, Line Spectra, O Stars, Radiation Pressure, Stellar Mass Ejection, Stellar Winds, Emission Spectra, Main Sequence Stars, Molecular Oscillators, Optical Thickness, Stellar Atmospheres, Stellar Evolution, Stellar Spectra
DOI:
10.1086/153315
Bibliographic Code:
1975ApJ...195..157C

Abstract

The large number of subordinate lines of a representative ion are found to have a dominant effect on the force of radiation on material in O star atmospheres. The force is increased over that due to resonance lines alone so that rates of mass loss are obtained which are 100 times greater than previously thought possible. The force is related to the solution of the line-transfer problem, and it becomes a function of the local velocity gradient. A new stellar wind theory, with a different interpretation of the singular point, is developed to treat this situation. The rate of mass loss, and other properties of the model, are uniquely specified by the luminosity, mass, and radius of the star. Alternative static models do not exist. Numerical results give a rate of mass loss equal to .000006 solar mass per year for an O5 star, with a terminal velocity of 1500 km/sec. The rate of mass loss is sensitive to stellar parameters, while the terminal velocity is not.

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)

  New!

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