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Title:
X-Ray Spectroscopy of SN 1006 with Suzaku
Authors:
Yamaguchi, Hiroya; Koyama, Katsuji; Katsuda, Satoru; Nakajima, Hiroshi; Hughes, John P.; Bamba, Aya; Hiraga, Junko S.; Mori, Koji; Ozaki, Masanobu; Tsuru, Takeshi Go
Affiliation:
AA(Department of Physics, Kyoto University, Kitashirakawa-oiwake-cho, Sakyo-ku, Kyoto 606-8502; ), AB(Department of Physics, Kyoto University, Kitashirakawa-oiwake-cho, Sakyo-ku, Kyoto 606-8502), AC( Department of Earth and Space Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043), AD( Department of Earth and Space Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043), AE( Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USA), AF(Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510), AG(RIKEN The Institute of Physical and Chemical Research, 2-1 Hirosawa, Wako, Saitama 351-0198), AH(Department of Applied Physics, University of Miyazaki, 1-1 Gakuen Kibana-dai, Nishi Miyazaki, Miyazaki 889-2192), AI(Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510), AJ(Department of Physics, Kyoto University, Kitashirakawa-oiwake-cho, Sakyo-ku, Kyoto 606-8502)
Publication:
Publications of the Astronomical Society of Japan, Vol.60, No.SP1, pp.S141--S152 (PASJ Homepage)
Publication Date:
01/2008
Origin:
PASJ
Keywords:
supernovae: individual(SN 1006), X-rays:spectra
Bibliographic Code:
2008PASJ...60S.141Y

Abstract

We report on observations of SN 1006 with Suzaku. We firmly detected K-shell emission from Fe, for the first time, and found that the Fe ionization state is quite low. The broad-band spectrum extracted from southeast of the remnant was well-fitted with a model consisting of three optically thin thermal non-equilibrium ionization plasmas and a power-law component. Two of the thermal models are highly overabundant in heavy elements, and hence are likely due to ejecta. These components have different ionization parameters, net ˜1.4 × 1010 cm-3s and net ˜ 7.7 × 108 cm-3s; it is the later one that produces Fe-K emission. This suggests that Fe has been heated by reverse shock more recently than the other elements, consistent with a picture where the ejecta are stratified by composition with Fe in the interior. On the other hand, the third thermal component is assumed to be solar abundance, and we associate it with emission from the interstellar medium. The electron temperature (kTe ˜ 0.5keV) is lower than that expected from the shock velocity, which suggests a lack of collisionless electron heating at the forward shock. The extremely low ionization parameter and extreme non-equilibrium state are due to the low density of the ambient medium.
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