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A Flare in the Jet of Pictor A

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arxiv 1004.0191 v1 pith:UJ2EDAFJ submitted 2010-04-01 astro-ph.HE

H. L. Marshall , M.J. Hardcastle , M. Birkinshaw , J. Croston , D. Evans , H. Landt , E. Lenc , F. Massaro
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E. S. Perlman D. A. Schwartz A. Siemiginowska {L}. Stawarz C. M. Urry D.M. Worrall
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classification astro-ph.HE
keywords x-rayfeatureflareobservationobservedpictorsynchrotronvariability
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A Chandra X-ray imaging observation of the jet in Pictor A showed a feature that appears to be a flare that faded between 2000 and 2002. The feature was not detected in a follow-up observation in 2009. The jet itself is over 150 kpc long and a kpc wide, so finding year-long variability is surprising. Assuming a synchrotron origin of the observed high-energy photons and a minimum energy condition for the outflow, the synchrotron loss time of the X-ray emitting electrons is of order 1200 yr, which is much longer than the observed variability timescale. This leads to the possibility that the variable X-ray emission arises from a very small sub-volume of the jet, characterized by magnetic field that is substantially larger than the average over the jet.

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