Ionization and Velocity Structure in the Supernova Remnant E0102-72

Details Ionization and Velocity Structure in the Supernova Remnant E0102-72 Ionization and Velocity Structure in the Supernova Remnant E0102-72

2001-05-03

arxiv.org/abs/astro-ph/0105058v1

Astronomy and Astrophysics

Astrophysics

8 pages, 9 figures; To appear in the ASP Conference Series for X-ray Astronomy 2000, Palermo Italy, eds. Giacconi, Stella & Se

Scientific paper

The High Energy Transmission Grating (HETG) Spectrometer aboard the Chandra X-Ray Observatory was used to observe E0102-72, a ~1000 year old, oxygen rich supernova in the Small Magellanic Cloud. The HETG disperses the image of the remnant into a spectrum of images in the light of individual X-ray emission lines. Doppler shifts in the strongest lines of oxygen and neon reveal bulk motions of up to 2000 km/sec with a complex morphology. Comparison of progressive ionization stages of magnesium, neon, oxygen and silicon provide new insights into the mechanism of the `reverse shock' that heats the stellar ejecta.

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