Ionization and Velocity Structure in the Supernova Remnant E0102-72

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dc.creatorFlanagan, K. A.
dc.creatorCanizares, C. R.
dc.creatorDavis, D. S.
dc.creatorDewey, D.
dc.creatorHouck, J. C.
dc.creatorMarkert, T. H.
dc.creatorSchattenburg, M. L.
dc.date2001-05-03
dc.date.accessioned2026-07-25T11:32:42Z
dc.descriptionThe 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.
dc.description8 pages, 9 figures; To appear in the ASP Conference Series for X-ray Astronomy 2000, Palermo Italy, eds. Giacconi, Stella & Serio
dc.identifierhttps://arxiv.org/abs/astro-ph/0105058
dc.identifierhttp://arxiv.org/abs/astro-ph/0105058
dc.identifier.urihttps://dspace.dare.co.zw/handle/123456789/3596
dc.subjectAstrophysics
dc.titleIonization and Velocity Structure in the Supernova Remnant E0102-72
dc.typetext

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