Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A
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2019-01-22
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Bradford Snios, Sarka Wykes, Paul E. J. Nulsen, Ralph P. Kraft, Eileen T. Meyer, Mark Birkinshaw, Diana M. Worrall, Martin J. Hardcastle, Elke Roediger, William R. Forman, Christine Jones , Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A, The Astrophysical Journal, Volume 871, Number 2; https://iopscience.iop.org/article/10.3847/1538-4357/aafaf3
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© 2019. The American Astronomical Society. All rights reserved.
© 2019. The American Astronomical Society. All rights reserved.
Abstract
We report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 years, collective proper motion of 11.3±3.3 mas yr We report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 years, collective proper motion of 11.3±3.3 mas yr −1 , or 0.68±0.20c , is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of 0.10c . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material. , or 0.68±0.20c , is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of 0.10c . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material.