Ionization Structure and the Reverse Shock in E0102-72

Details Ionization Structure and the Reverse Shock in E0102-72 Ionization Structure and the Reverse Shock in E0102-72

2001-05-02

arxiv.org/abs/astro-ph/0105040v2

Astronomy and Astrophysics

Astrophysics

4 pages, 6 figures; To appear in "Young Supernova Remnants" (11th Annual Astrophysics Conference in Maryland), S. S. Holt & U.

Scientific paper

10.1063/1.1377098

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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