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/0509911)
· On-line Data
· References in the article
· Citations to the Article (12) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Shock-cloud interaction in the Vela SNR observed with XMM-Newton
Authors:
Miceli, M.; Bocchino, F.; Maggio, A.; Reale, F.
Affiliation:
AA(Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy ), AB(INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy), AC(INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy), AD(Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy)
Publication:
Astronomy and Astrophysics, Volume 442, Issue 2, November I 2005, pp.513-525 (A&A Homepage)
Publication Date:
11/2005
Origin:
EDP Sciences
Keywords:
X-rays: ISM, ISM: supernova remnants, ISM: clouds, ISM: kinematics and dynamics, ISM: individual objects: Vela SNR
DOI:
10.1051/0004-6361:20041919
Bibliographic Code:
2005A&A...442..513M

Abstract

We analyzed an XMM-Newton EPIC observation of a bright knot, named FilD, in the northern rim of the Vela SNR, where the shock has encountered a cloud. The good combination of sensitivity, spectral, and spatial resolution allowed us to describe the internal structure of the observed ISM clouds and to obtain estimates of their temperature, density, O, Ne, and Fe abundances, and of their extension along the line of sight. We also examined the interaction of the shock with the FilD knot and estimated that the time elapsed from the shock impact is about one cloud crushing time. Our analysis allowed us to conclude that the observed X-ray emission is best explained by the propagation of transmitted shocks through ISM inhomogeneities with an inward increasing density profile. We found that the interaction with the shock determines the heating of the inner part of the clouds and the evaporation of the outer part.

Associated Articles

Part 1     Part  2    

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