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dc.contributor.authorMarshall, Herman L.
dc.contributor.authorHardcastle, Martin J.
dc.contributor.authorBirkinshaw, Mark
dc.contributor.authorCroston, Judith H.
dc.contributor.authorEvans, Daniel A.
dc.contributor.authorLandt, Hermine
dc.contributor.authorLenc, Emil
dc.contributor.authorMassaro, Francesco
dc.contributor.authorPerlman, Eric S.
dc.contributor.authorSchwartz, Daniel A.
dc.date.accessioned2014-12-04T18:33:25Z
dc.date.available2014-12-04T18:33:25Z
dc.date.issued2010-04-13
dc.identifier.citationCroston, J., Evans, D., Lenc, E., Landt, H., Perlman, E.S., et. al. (2010) A flare in the jet of pictor A. The Astrophysical Journal Letters, 714(2), L213.en_US
dc.identifier.urihttp://hdl.handle.net/11141/455
dc.description.abstractA 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 150kpc long and about 1 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 years, 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 a magnetic field that is substantially larger than the average over the jet.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. Copyright Law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titleA flare in the jet of pictor Aen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/2041-8205/714/2/L213


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