期刊
ASTRONOMY & ASTROPHYSICS
卷 365, 期 1, 页码 L242-L247出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20000082
关键词
atomic processes; line : formation; line : identification; techniques : spectroscopic; supernovae : individual : N132D; ISM : supernova remnants
The observation of the supernova remnant N132D by the scientific instruments oil board the XMM-Newton satellite is presented. The X-rays from N132D are dispersed into a detailed line-rich spectrum using the Reflection Grating Spectrometers. Spectral lines of C, N, O Ne, Mg, Si, S, and Fe are identified. images of the remnant, in narrow wavelength bands, produced by the European Photon Imaging Cameras reveal a complex spatial structure of the ionic distribution. While K-shell Fe emission seems to originate near the centre, all of the other ions are observed along the shell. A high O6+/O7+ emission ratio is detected on the northeastern edge of the remnant. This can be a sign of hot ionising conditions, or it can reflect relatively cool gas. Spectral fitting of the CCD spectrum suggests high temperatures in this region, but a detailed analysis of the atomic processes involved in producing the O6+ spectral lines leads to the conclusion that the intensities of these lines alone cannot provide a conclusive distinction between the two scenarios.
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