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Title:
Chandra X-Ray Observatory Study of Vela Shrapnel A
Authors:
Miyata, Emi; Tsunemi, Hiroshi; Aschenbach, Bernd; Mori, Koji
Affiliation:
AA(; Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, 560-0043 Osaka, Japan; , , .), AB(; Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, 560-0043 Osaka, Japan; , , .), AC(; Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse Postfach 1312, D-85741 Garching, Germany; .), AD(; Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, 560-0043 Osaka, Japan; , , .; Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.)
Publication:
The Astrophysical Journal, Volume 559, Issue 1, pp. L45-L48. (ApJL Homepage)
Publication Date:
09/2001
Origin:
UCP
ApJ Keywords:
ISM: Abundances, ISM: Individual: Name: Vela Supernova Remnant, ISM: Supernova Remnants, X-Rays: ISM
DOI:
10.1086/323653
Bibliographic Code:
2001ApJ...559L..45M

Abstract

We present high-resolution Chandra observations of shrapnel A in the vicinity of the Vela supernova remnant. The Chandra image reveals a bright X-ray region at the head position of shrapnel A and a fainter extended tail. The spectral analysis shows that the plasma is in a condition of nonequilibrium ionization. The abundance of O is 0.34+0.12-0.08 times that of the solar value, whereas that of Si is 3+2-1 times solar, showing an anomalous abundance ratio for the two elements. The ionization timescale indicates that the shrapnel had been heated up about 104 yr ago. We confirm that the pressure in the head region is ~=10 times higher than that in the tail region, which is not explained by a simple blast-wave model. These facts strongly support the view that shrapnel A is a fragment of the progenitor star created in the supernova explosion.
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