Ionization Structure and the Reverse Shock in E0102-72
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.
Cite
@article{arxiv.astro-ph/0105040,
title = {Ionization Structure and the Reverse Shock in E0102-72},
author = {K. A. Flanagan and C. R. Canizares and D. S. Davis and D. Dewey and J. C. Houck and M. L. Schattenburg},
journal= {arXiv preprint arXiv:astro-ph/0105040},
year = {2009}
}
Comments
4 pages, 6 figures; To appear in "Young Supernova Remnants" (11th Annual Astrophysics Conference in Maryland), S. S. Holt & U. Hwang (eds), AIP, New York (2001)