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Ionization Structure and the Reverse Shock in E0102-72

K. A. Flanagan·C. R. Canizares·D. S. Davis·D. Dewey·J. C. Houck·M. L. Schattenburg
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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.

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K. A. Flanagan, C. R. Canizares, D. S. Davis, D. Dewey, J. C. Houck, M. L. Schattenburg. 2001-05-03. Ionization Structure and the Reverse Shock in E0102-72. https://doi.org/10.1063/1.1377098

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