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/0104384)
· References in the article
· Citations to the Article (11) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
A high frequency radio study of G11.2-0.3, a historical supernova remnant with a flat spectrum core
Authors:
Kothes, R.; Reich, W.
Affiliation:
AA(National Research Council, Herzberg Institute of Astrophysics, Dominion Radio Astrophysical Observatory, PO Box 248, Penticton, British Columbia, V2A 6K3, Canada), AB(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany )
Publication:
Astronomy and Astrophysics, v.372, p.627-635 (2001) (A&A Homepage)
Publication Date:
06/2001
Origin:
A&A
A&A Keywords:
SUPERNOVA REMNANT, MAGNETIC FIELD, RADIO CONTINUUM: ISM
DOI:
10.1051/0004-6361:20010407
Bibliographic Code:
2001A&A...372..627K

Abstract

We present radio maps of the historical supernova remnant G11.2-0.3 in the frequency range from 4.85 GHz to 32 GHz. The integrated spectrum with alpha = -0.50 (S ~ nu \alpha) is dominated by its steep spectrum shell emission (alpha ~ -0.57), although a flat spectrum core structure classifies G11.2-0.3 as a composite supernova remnant. A radial magnetic field structure is observed. An analysis of the multi-frequency polarization data results in highly varying rotation measures along the shell. The percentage polarization is rather low ( ~ 2%) and we conclude that G11.2-0.3 is in the transient phase from free to adiabatic expansion. The central flat spectrum component is partly resolved. A compact radio source with an inverted spectrum likely coincides with the previously detected X-ray pulsar (Torii et al. \cite{torii1997}). Two symmetric structures with flat radio spectra possibly indicate a bipolar outflow. Combining available X-ray and radio data we conclude that G11.2-0.3 is likely the remnant of a type II supernova explosion with an early type B progenitor star.
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