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Title:
Spatially Resolved Spectral Analysis of Vela Shrapnel D
Authors:
Katsuda, Satoru; Tsunemi, Hiroshi
Affiliation:
AA(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043; ), AB(Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043; )
Publication:
Publications of the Astronomical Society of Japan, Vol.57, No.4, pp. 621-628 (PASJ Homepage)
Publication Date:
08/2005
Origin:
PASJ
Keywords:
ISM: abundances, ISM: individual (Vela Supernova Remnant), supernova remnants, X-rays: ISM
Bibliographic Code:
2005PASJ...57..621K

Abstract

The ROSAT all-sky survey discovered several `shrapnels', showing boomerang structures outside the Vela supernova remnant. We observed shrapnel D with the XMM-Newton satellite. There is an X-ray bright ridge structure in our FOV running from north to south. Applying the VNEI model to X-ray spectra of various regions, we find that the plasma in the eastern part from the X-ray ridge is significantly different from that in the western part. The X-ray spectra in the western part can be represented by a single-temperature component. The abundances of heavy elements are almost uniform, whereas they are heavily overabundant, except for Fe; the relative abundances to the solar values are O ˜ 5, Ne ˜ 10, Mg ˜ 10, Fe ˜ 1. This indicates that shrapnel D originated from the ejecta of the supernova. We find that the plasma in the eastern part from the ridge consists of two components with different temperatures; the hot component comes from the ejecta, while the cold component comes from the interstellar matter. These two components are considered to be in contact with each other, forming a contact discontinuity. Around the northern part of the contact discontinuity, we find wave-like structures of which the typical scale are comparable with that of the Rayleigh-Taylor instability.
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