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 (14) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The polarization and depolarization of radio emission from supernova remnant Cassiopeia A
Authors:
Anderson, M. C.; Keohane, J. W.; Rudnick, L.
Affiliation:
AA(University of Minnesota, Minneapolis, MN, US), AB(University of Minnesota, Minneapolis, MN, US), AC(University of Minnesota, Minneapolis, MN, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 441, no. 1, p. 300-306 (ApJ Homepage)
Publication Date:
03/1995
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
CASSIOPEIA A, DEPOLARIZATION, MAGNETOHYDRODYNAMICS, POLARIZATION (WAVES), RADIO SOURCES (ASTRONOMY), SHOCK WAVES, SUPERNOVAE, ASTRONOMICAL POLARIMETRY, MAGNETIC FIELDS, RELATIVISTIC PLASMAS, SYNCHROTRON RADIATION, X RAYS
DOI:
10.1086/175356
Bibliographic Code:
1995ApJ...441..300A

Abstract

We present a study of polarimetric images of the supernova remnant Cassiopeia A at observing wavelengths of lambda = 6 and 20 cm. We find that the brigth ring is strongly depolarized at lambda = 20 cm and conclude that this is due to a mixing of the relativistic plasma responsible for the synchrotron emission and the thermal soft X-ray-emitting material behind the reverse shock. On large scales, the magnetic field is radial in Cas A, as is common in young remnants. However, the radial field region extends well beyond the bright ring, putting constraints on the field-generating mechanism. Two interesting types of small-scale features are also found and probably reflect the same underlying phenomena; the first are features at lambda = 20 cm that appear to have penetrated beyond the Faraday depolarizing shell, and the second are regions of small-scale variations in the magnetic field direction at lambda = 6 cm. Both of these are likely to be identified with moderately dense clumps of stellar ejecta, leading to the bow shocks discussed by Braun, Gull, & Perley (1987) and the evolving compact features discussed by Anderson & Rudnick (1995a).

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