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)
· arXiv e-print (arXiv:astro-ph/0007365)
· On-line Data
· References in the article
· Citations to the Article (23) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (8)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Discovery of Non-Thermal X-Rays from the Shell of RCW 86
Authors:
Bamba, Aya; Koyama, Katsuji; Tomida, Hiroshi
Affiliation:
AA(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502; ), AB(Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502; CREST, Japan Science and Technology Corporation (JST), 4-1-8 Honmachi, Kawaguchi, Saitama 332-0012), AC(National Space Development Agency of Japan, World Trade Center Building, 2-4-1 Hamamatsu-cho, Minato-ku, Tokyo 105-8060})
Publication:
Publ. of the Astronomical Society of Japan, v.52, p.1157-L1163. (PASJ Homepage)
Publication Date:
12/2000
Origin:
PASJ
PASJ Keywords:
ACCELERATION OF PARTICLES, ISM: INDIVIDUAL (RCW 86), SUPERNOVA REMNANTS, X-RAYS: ISM
Bibliographic Code:
2000PASJ...52.1157B

Abstract

We report the ASCA (Advanced Satellite for Cosmology and Astrophysics) results of RCW 86, a shell-like supernova remnant (SNR). The bright region in the X-ray band traces the radio clumpy shell, although details of the structure are different. The X-ray spectrum from each part of the shell can not be fitted to a thin thermal plasma model, but requires at least three components: a low-temperature plasma of 0.3 keV, a high-temperature plasma of >= several keV, and a power-law component with a photon index of ~ 3. The abundances of O, Ne, Mg, and Si are significantly higher than that of Fe, indicating that RCW 86 is a type II SNR. The absorption column of ~ 3times 1021 H cm-2 indicates the distance to the SNR to be several kpc. The power-law component can be interpreted to be synchrotron radiation of high-energy electrons. Assuming an energy density equipartition between the magnetic field and the electrons, and using the radio and X-ray spectra, we argue that high-energy electrons are accelerated up to 20 TeV. The acceleration efficiency is, however, different from shell to shell.

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