http://arxiv.org/abs/1805.05951
We present an interpretation of the time variability of the $X$-ray flux recently reported from a multi-epoch campaign of $15$ years observations of the supernova remnant Cassiopeia A by {\it Chandra}. We show for the first time quantitatively that the $[4.2-6]$ keV non-thermal flux increase up to $50\%$ traces the growth of the magnetic field due to vortical amplification mechanism at a reflection inward shock colliding with inner overdensities. The fast synchrotron cooling as compared with shock-acceleration time scale qualitatively supports the flux decrease.
F. Fraschetti, S. Katsuda, T. Sato, et. al.
Thu, 17 May 18
66/70
Comments: 5 pages, 2 figures, PRL in press
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