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 (102) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Expansion of a superbubble in a uniform magnetic field
Authors:
Ferriere, Katia M.; Mac Low, Mordecai-Mark; Zweibel, Ellen G.
Affiliation:
AA(Colorado, University; Joint Institute for Laboratory Astrophysics, Boulder), AB(NASA, Ames Research Center, Moffett Field, CA), AC(Colorado, University, Boulder)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 375, July 1, 1991, p. 239-253. (ApJ Homepage)
Publication Date:
07/1991
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Bubbles, Interstellar Magnetic Fields, Interstellar Matter, Magnetohydrodynamics, Shock Wave Propagation, Supernovae, Analytic Functions, Computational Astrophysics, Expansion, Numerical Analysis
DOI:
10.1086/170185
Bibliographic Code:
1991ApJ...375..239F

Abstract

The effects of interstellar magnetic fields on the evolution and structure of superbubbles are investigated. First, the governing equations for propagation of a radiative shock are derived and solved analytically in the limit of high expansion velocity. A numerical code able to solve them in the general case and discuss the numerical results is then presented. It is found that magnetic fields of the strength present in the Galactic disk do not significantly modify the overall shape and dimensions of a superbubble. They reduce the volume of the interior cavity by one-third on average during the expansion phase. The shell elongates slightly in the direction of the external field. Magnetic pressure dominates over gas pressure in most of the shell and forces it to thicken substantially. Finally, because of the transverse mass motions which take place from the magnetic poles to the equator, the column density at the poles is reduced by typically a factor of 10.

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