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Title:
An X-ray map of SN 1006 from the Einstein Observatory
Authors:
Pye, J. P.; Pounds, K. A.; Rolf, D. P.; Smith, A.; Willingale, R.; Seward, F. D.
Affiliation:
AA(Leicester, University, Leicester, Leics., England), AB(Leicester, University, Leicester, Leics., England), AC(Leicester, University, Leicester, Leics., England), AD(Leicester, University, Leicester, Leics., England), AE(Leicester, University, Leicester, Leics., England), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.)
Publication:
Royal Astronomical Society, Monthly Notices, vol. 194, Feb. 1981, p. 569-582. Research supported by the Science Research Council; (MNRAS Homepage)
Publication Date:
02/1981
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ASTRONOMICAL MAPS, SUPERNOVA REMNANTS, X RAY IMAGERY, X RAY SOURCES, X RAY SPECTRA, ASTRONOMICAL OBSERVATORIES, BRIGHTNESS, EMISSION SPECTRA, IMAGE RESOLUTION, PROPORTIONAL COUNTERS, SPACE PLASMAS, THREE DIMENSIONAL MODELS
Comment:
A&AA ID. AAA029.125.001
Bibliographic Code:
1981MNRAS.194..569P

Abstract

An X-ray map of the SN 1006 supernova remnant acquired by the imaging proportional counter of the Einstein Observatory in the energy range 0.1-4 keV is presented. The image obtained from the imaging proportional counter shows a limb-brightened nebula, almost circular in outline with enhanced emission in two quadrants. The hardness ratio map reveals a large range of temperatures over the object, with the highest values near the limbs of the enhanced emission regions. Consideration of a three-dimensional model of the object indicates the presence of a shell of electron temperature varying between 10 to the 6th and 10 to the 7th K and density varying between 0.3 and 6/cu cm surrounding a fairly uniform interior, of electron temperature 1.5 x 10 to the 6th K and density 1.0/cu cm. The optical filaments are observed to lie parallel with the faintest edge of the X-ray shell, about 1 arcmin from the peak of X-ray emission. Mass visible in the X-ray image of 5-15 solar masses suggests that the supernova may have been of type II. No evidence is obtained for a hot stellar remnant.

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