Disk evolution of the M87’s nucleus observed in 2008. (arXiv:2002.09122v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Xiang_F/0/1/0/all/0/1">Fei Xiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_C/0/1/0/all/0/1">Cheng Cheng</a>
We report the discovery of year-scale X-ray variation in the nuclear region
of the M87 by reanalyzing the 8 Chandra observations from 2007 to 2008. The
X-ray spectra are fitted and decomposed into the disk and flaring components.
This year-scale X-ray variability can be explained quite well by a simple
clumpy accretion model. We conclude that the central super-massive black hole
of the M87 was accreting a cloud of $sim0.5$M$_odot$ at that time.
We report the discovery of year-scale X-ray variation in the nuclear region
of the M87 by reanalyzing the 8 Chandra observations from 2007 to 2008. The
X-ray spectra are fitted and decomposed into the disk and flaring components.
This year-scale X-ray variability can be explained quite well by a simple
clumpy accretion model. We conclude that the central super-massive black hole
of the M87 was accreting a cloud of $sim0.5$M$_odot$ at that time.
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