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 (1183) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Interstellar bubbles. II - Structure and evolution [ Erratum: 1978ApJ...220..742W ]
Authors:
Weaver, R.; McCray, R.; Castor, J.; Shapiro, P.; Moore, R.
Affiliation:
AA(Colorado, University; Joint Institute for Laboratory Astrophysics, Boulder, Colo.), AB(Colorado, University; Joint Institute for Laboratory Astrophysics, Boulder, Colo.), AC(Colorado, University; Joint Institute for Laboratory Astrophysics, Boulder, Colo.), AD(Harvard College Observatory and Smithsonian Astrophysical Observatory, Center for Astrophysics, Cambridge, Mass.)
Publication:
Astrophysical Journal, Part 1, vol. 218, Dec. 1, 1977, p. 377-395. (ApJ Homepage)
Publication Date:
12/1977
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
INTERSTELLAR GAS, PLASMA INTERACTIONS, STELLAR WINDS, ADIABATIC FLOW, BUBBLES, CONDUCTIVE HEAT TRANSFER, EARLY STARS, ENERGY DISSIPATION, HYDRODYNAMICS, ION DENSITY (CONCENTRATION), RADIATIVE TRANSFER, STELLAR MOTIONS
Comment:
A&AA ID. AAA020.064.037
DOI:
10.1086/155692
Bibliographic Code:
1977ApJ...218..377W

Abstract

The detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented. First, an adiabatic similarity solution is given which is applicable at early times. Second, a similarity solution is derived which includes the effects of thermal conduction between the hot (about 1 million K) interior and the cold shell of swept-up interstellar matter. This solution is then modified to include the effects of radiative energy losses. The evolution of an interstellar bubble is calculated, including the radiative losses. The quantitative results for the outer-shell radius and velocity and the column density of highly ionized species such as O VI are within a factor 2 of the approximate results of Castor, McCray, and Weaver (1975). The effect of stellar motion on the structure of a bubble, the hydrodynamic stability of the outer shell, and the observable properties of the hot region and the outer shell are discussed.

Associated Articles

Part  1     Main Paper     Erratum    

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