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Ionization Structure and the Reverse Shock in E0102-72

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 نشر من قبل Kathryn Flanagan
 تاريخ النشر 2001
  مجال البحث فيزياء
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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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