Einstein observations of the VELA supernova remnant - The spatial structure of the hot emitting gas

Details Einstein observations of the VELA supernova remnant - The spatial structure of the hot emitting gas Einstein observations of the VELA supernova remnant - The spatial structure of the hot emitting gas

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299..821k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 15, 1985, p. 821-827.

Astronomy and Astrophysics

Astrophysics

45

Heao 2, Nebulae, Supernova Remnants, X Ray Sources, X Ray Spectra, Spectrum Analysis

Scientific paper

Spatially resolved (aproximately 1 arcmin) X-ray maps of the Vela supernova remnant have been constructed in two spectral bands, 0.2-1.0 keV and 0.8-2.0 keV, from a series of 36 separate observations with the Imaging Proportional Counter of the Einstein Observatory. The maps exhibit substantial structure on all angular scales. Spectral analysis shows that the emission from the remnant can be consistently described as thermal radiation from hot gas which is nonuniform in density and temperature, but which is in approximate pressure equilibrium. It is found that p/k is approximately 3-4 x 10 to the 5th/cu cm K. The soft X-ray emission exhibits a high degree of correlation with the optical filamentary structure, in the sense that the most prominent filaments either tightly surround or are coincident with the brightest X-ray regions. This suggests that the softest X-radiation may originate in 'warm' gas which is evaporated from the denser clouds responsible for the optical and ultraviolet filaments. Such an interpretation is quantitatively investigated, and shown to be only marginally consistent with the observations.

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