A FLARE IN THE JET OF PICTOR A
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 about 1 kpc wide, so finding year-long variability is surp...
Main Authors: | , , , , , , , , , , , , , |
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Other Authors: | , |
Format: | Article |
Language: | English |
Published: |
Institute of Physics/American Astronomical Society,
2015-03-04T18:21:22Z.
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Subjects: | |
Online Access: | Get fulltext |
Summary: | 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 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. Poland. Ministry of Science and Higher Education (grant N-N203-380336) Smithsonian Astrophysical Observatory (SAO contract NAS 8-39073) Chandra X-ray Center (U.S.) (contract NAS8-03060) Smithsonian Astrophysical Observatory (SAO contract SV3-73016) |
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