Hard X-ray emission from the VELA supernova remnant

Details Hard X-ray emission from the VELA supernova remnant Hard X-ray emission from the VELA supernova remnant

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.254..139w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 254, Jan. 1, 1992, p. 139-145. Research supported by SE

Astronomy and Astrophysics

Astronomy

17

Pulsars, Spaceborne Astronomy, Supernova Remnants, Synchrotron Radiation, X Ray Sources, Nebulae, Spacelab Payloads, X Ray Spectra

Scientific paper

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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