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Flaring X-ray Emission from HST-1, a Knot in the M87 Jet

D. E. Harris·J. A. Biretta·W. Junor·E. S. Perlman·W. B. Sparks·A. S. Wilson
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Abstract

We present Chandra X-ray monitoring of the M87 jet in 2002, which shows that the intensity of HST-1, an optical knot 0.8" from the core, increased by a factor of two in 116 days and a factor of four in 2 yrs. There was also a significant flux decrease over two months, with suggestive evidence for a softening of the spectrum. From this variability behavior, we argue that the bulk of the X-ray emission of HST-1 comes from synchrotron emission. None of the other conceivable emission processes can match the range of observed characteristics. By estimating synchrotron model parameters for various bulk relativistic velocities, we demonstrate that a model with a Doppler factor, delta, in the range 2 to 5 fits our preliminary estimates of light travel time and synchrotron loss timescales.

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D. E. Harris, J. A. Biretta, W. Junor, E. S. Perlman, W. B. Sparks, A. S. Wilson. 2003-02-13. Flaring X-ray Emission from HST-1, a Knot in the M87 Jet. https://doi.org/10.1086/374773

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