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S. Park (Penn State), J. P. Hughes (Rutgers), P. O. Slane (CfA), D. N. Burrows, P. W. A. Roming, J. A. Nousek, G. P. Garmire (Penn State)
With the high angular resolution Chandra data, we resolved metal-rich ejecta knots and the shocked circumstellar medium (CSM) in the Galactic oxygen-rich supernova remnant (SNR) G292.0+1.8. X-ray emission from the ejecta material of G292.0+1.8 is dominated by highly ionized O, Ne and Mg. There is little evidence for such enriched Si, S, and Fe. This is in contrast to another Galactic O-rich SNR, Cas A, in which Fe and Si are abundant. Measured abundance ratios of the ejecta in G292.0+1.8 suggest that the bulk of the detected ejecta was generated in the outer layers of an ~25 Msun progenitor star. The bright equatorial belt is dominated by X-ray emission with normal abundances, which supports a shocked CSM origin. We find a significant pressure difference between the CSM and the associated pulsar wind nebula (PWN). The reverse shock thus appears not to have reached the central region of this young SNR, and so the Fe-rich ejecta there as well as the PWN, which might be responsible for the non-detection of Fe-rich ejecta in G292.0+1.8.
The author(s) of this abstract have provided an email address for comments about the abstract: park@astro.psu.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.