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/0407401)
· On-line Data
· References in the article
· Citations to the Article (26) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Spectral properties of nonthermal X-ray emission from the shell-type SNR RX J1713.7 3946 as revealed by XMM-Newton
Authors:
Hiraga, J. S.; Uchiyama, Y.; Takahashi, T.; Aharonian, F. A.
Affiliation:
AA(Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan ), AB(Yale Center for Astronomy & Astrophysics, PO Box 208121, New Haven, CT 06520-8121, USA), AC(Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan), AD(Max-Plank-Institut für Kernphysik, Postfach 103980, 69026 Heidelberg, Germany)
Publication:
Astronomy and Astrophysics, Volume 431, Issue 3, March I 2005, pp.953-961 (A&A Homepage)
Publication Date:
03/2005
Origin:
EDP Sciences
Keywords:
radiation mechanisms: non-thermal, ISM: supernova remnants, ISM: cosmic rays, stars: suparnovae: individual: RX J1713.7–3946
DOI:
10.1051/0004-6361:20047015
Bibliographic Code:
2005A&A...431..953H

Abstract

We present the results of our morphological and spectral study of the properties of the supernova remnant RX J1713.7-3946 based on data obtained with XMM-Newton. Highly inhomogeneous structures, such as the bright spots, filaments, and dark voids noted by Uchiyama et al. ([CITE]), appear in the entire bright western portion of the shell. In addition two narrow rims are found which run parallel to each other from north to south in the western part of the remnant. No complex structures are seen in the interior region of the remnant. The X-ray spectra everywhere can be well represented by a power-law function with photon index in the range within Γ = 2.0 2.8. A clear difference between spectra of the central dim region and of the bright western portion is seen at lower energies. This difference can be ascribed either to an additional thermal component in the center with electron temperature kT_e= 0.56~~keV or, alternatively, to an increase in column density by Δ N_H˜ 0.3× 1022~ cm-2 in the western region. In the context of the recent discovery by the NANTEN telescope of a molecular cloud apparently interacting with the western part of the supernova remnant the second possibility seems to be the more likely scenario.
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