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)
· arXiv e-print (arXiv:astro-ph/0008042)
· References in the article
· Citations to the Article (13) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (12)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The Radio Structure of the Supernova Remnant G315.4-2.3 (MSH 14-63)
Authors:
Dickel, John R.; Strom, Richard G.; Milne, D. K.
Affiliation:
AA(Astronomy Department, University of Illinois at Urbana-Champaign, Urbana, IL 61801), AB(ASTRON, 7990AA Dwingeloo, The Netherlands), AC(Australia Telescope National Facility, Epping NSW 1710, Australia)
Publication:
The Astrophysical Journal, Volume 546, Issue 1, pp. 447-454. (ApJ Homepage)
Publication Date:
01/2001
Origin:
UCP
ApJ Keywords:
Polarization, Radiation Mechanisms: Nonthermal, Radio Continuum: ISM, ISM: Supernova Remnants
DOI:
10.1086/318259
Bibliographic Code:
2001ApJ...546..447D

Abstract

G315.4-2.3 is an extended-shell supernova remnant (SNR) with some characteristics of evolutionarily young remnants and some of older ones. To further elucidate some of its characteristics, we present imaging and polarimetry of this SNR at a frequency of 1.34 GHz with a resolution of 8" made with the Australia Telescope Compact Array. The indicators of youth are as follows: (1) morphologically, the radio emission arises in a smooth shell without the fine-scale filaments seen in the optical; (2) many of the optical filaments are Balmer dominated; (3) where measurable, the orientation of the magnetic field appears to be radial with respect to the center of the remnant; and (4) there may have been a supernova in that region in AD 185. Indications of older age include the following: (1) particularly in RCW 86, the bright optical nebula in the southwestern corner of this extended SNR, but also in other locations there are several filaments with bright [S II] emission representative of older shocked filaments in radiative equilibrium and (2) if the remnant lies at the kinematical distance of 2.8 kpc, it has a diameter of 37 pc which would be large for a remnant less than 2000 years old. The remnant seems to be expanding inside a cavity outlined by infrared emission, and so it could well be young and large. Where it is encountering the walls of the cavity it is slowing rapidly, and we observe the radiative filaments. RCW 86 itself is encountering a dense clump of material but may also be the remains of a more compact lump of ejecta ploughing into the surroundings.
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