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Einstein observations of the Vela supernova remnant - The spatial structure of the hot emitting gasSpatially 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.
Document ID
19860049336
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Kahn, S. M.
(California, University Berkeley, United States)
Gorenstein, P.
(California Univ. Berkeley, CA, United States)
Harnden, F. R., Jr.
(California Univ. Berkeley, CA, United States)
Seward, F. D.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 12, 2013
Publication Date
December 15, 1985
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 299
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
86A34074
Funding Number(s)
CONTRACT_GRANT: NAS8-30753
CONTRACT_GRANT: NAS8-30751
Distribution Limits
Public
Copyright
Other

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