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Ionization Structure and the Reverse

By Shock In E and M. L. Schattenburg

Abstract

Abstract. The young oxygen-rich supernova remnant E0102-72 in the Small Magellanic Cloud has been observed with the High Energy Transmission Grating Spectrometer of Chandra. The high resolution X-ray spectrum reveals images of the remnant in the light of individual emission lines of oxygen, neon, magnesium and silicon. The peak emission region for hydrogen-like ions lies at larger radial distance from the SNR center than the corresponding helium-like ions, suggesting passage of the ejecta through the ”reverse shock”. We examine models which test this interpretation, and we discuss the implications. BACKGROUND 1E0102.2-7219 (hereinafter referred to as E0102-72) is a young (∼1000 years) oxygen-rich supernova remnant (SNR) in the Small Magellanic Cloud. E0102-72 has been observed at all wavelengths: in the optical [1] [2], UV [3] [4] , radio [5]

Year: 2001
OAI identifier: oai:CiteSeerX.psu:10.1.1.315.5599
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