Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (59) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (28)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Non-thermal emission in Wolf-Rayet stars: are massive companions required?
Authors:
Dougherty, S. M.; Williams, P. M.
Affiliation:
AA(National Research Council of Canada, Herzberg Institute for Astrophysics, Dominion Radio Astrophysical Observatory, PO Box 248, White Lake Rd, Penticton, British Columbia V2A 6K3, Canada ; Department of Physics and Astronomy, University of Calgary, 2500 University Dr. NW, Calgary, Alberta T2N 1N4, Canada ), AB(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 319, Issue 4, pp. 1005-1010. (MNRAS Homepage)
Publication Date:
12/2000
Origin:
MNRAS
MNRAS Keywords:
STARS: INDIVIDUAL: WR86, STARS: WOLF-RAYET, RADIO CONTINUUM: STARS
DOI:
10.1046/j.1365-8711.2000.03837.x
Bibliographic Code:
2000MNRAS.319.1005D

Abstract

We examine the radio spectral indices of 23 Wolf-Rayet (WR) stars to identify the nature of their radio emission. We identify nine systems as non-thermal emitters. In seven of these systems the non-thermal emission dominates the radio spectrum, while in the remaining two it is of comparable strength to the thermal, stellar wind emission, giving `composite' spectra. Among these nine systems, seven have known spectroscopic or visual binary companions. The companions are all massive O or early B-type stars, strongly supporting a connection between the appearance of non-thermal emission in WR stars and the presence of a massive companion. In three of these binaries, the origin of non-thermal emission in a wind-collision region between the stars has been well established in earlier work. The binary systems that exhibit only thermal emission are all short-period systems where a wind-collision zone is deep within the opaque region of the stellar wind of the WR star. To detect non-thermal emission in these systems requires optically thin lines of sight to the wind-collision region.

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