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Precessing Jet Model for the Supernova Remnant G109.1–1.0

Published online by Cambridge University Press:  04 August 2017

P. C. Gregory  and
G. G. Fahlman
P. C. Gregory
Affiliation:
Department of Physics, University of British Columbia, Vancouver, British Columbia, V6T 2A6
G. G. Fahlman
Affiliation:
Department of Geophysics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 2A6

Extract

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We propose that the central X-ray pulsar in G109.1–1.0, designated 1E 2259+586, ejects two oppositely directed precessing jets or beams, which give rise to the observed radio structure. The radio emission is interpreted as synchrotron emission from electrons accelerated at the interface of the jets with the walls of the SNR. Thus the observed intersecting arcs of radio emission represent the trace of the precessing jets on the supernova remnant walls. The precession axis is inclined at 37 degrees to the line of sight and the precession cone half angle is 55 degrees. The observed large scale X-ray jet in G109.1–1.0 is found to coincide in position with the precession axis as was found for the X-ray jets from SS 433.

Type
V. Compact Objects Associated With Supernova Remnants, Pulsars and Neutron Stars
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 429 - 436
Copyright
Copyright © Reidel 1983 

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