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Title:
Hard X-ray emission from the VELA supernova remnant
Authors:
Willmore, A. P.; Eyles, C. J.; Skinner, G. K.; Watt, M. P.
Affiliation:
AA(Birmingham, University, England), AB(Birmingham, University, England), AC(Birmingham, University, England), AD(Birmingham, University, England)
Publication:
Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 254, Jan. 1, 1992, p. 139-145. Research supported by SERC. (MNRAS Homepage)
Publication Date:
01/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
PULSARS, SPACEBORNE ASTRONOMY, SUPERNOVA REMNANTS, SYNCHROTRON RADIATION, X RAY SOURCES, NEBULAE, SPACELAB PAYLOADS, X RAY SPECTRA
Bibliographic Code:
1992MNRAS.254..139W

Abstract

Consideration is given to the first hard (2.5-25 keV) X-ray images of the Vela supernova remnant (SNR), resulting from observations with the University of Birmingham coded mask telescope flown on the Spacelab 2 mission in 1985. The emission from the region around the pulsar is resolved; the diffuse emission extends approximately 1 deg to the north-east and south-west, roughly aligned along the direction of the pulsar spin axis, and produces about 48 percent of the total emission in the 4-25 keV band. It is suggested that this region, which overlaps the peak of the Vela-X radio source, is a synchrotron nebula. The power required to produce the relativistic electrons in the nebula is estimated to be 75 percent of the rotational energy loss of the pulsar. Emission from a number of bright knots in the shell is also detected; while these generally correlate with bright features in the lower energy Einstein Observatory and the H-alpha images, the features at different wavelengths are not coincident, suggesting the presence of blobs of material at a wide range of temperatures.

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