On the impact of an intermediate duration X-ray burst on the accretion environment in IGR J17062-6143. (arXiv:2107.13543v1 [astro-ph.HE])

On the impact of an intermediate duration X-ray burst on the accretion environment in IGR J17062-6143. (arXiv:2107.13543v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bult_P/0/1/0/all/0/1">Peter Bult</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altamirano_D/0/1/0/all/0/1">Diego Altamirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arzoumanian_Z/0/1/0/all/0/1">Zaven Arzoumanian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballantyne_D/0/1/0/all/0/1">David R. Ballantyne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chenevez_J/0/1/0/all/0/1">Jerome Chenevez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabian_A/0/1/0/all/0/1">Andrew C. Fabian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gendreau_K/0/1/0/all/0/1">Keith C. Gendreau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Homan_J/0/1/0/all/0/1">Jeroen Homan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaisawal_G/0/1/0/all/0/1">Gaurava K. Jaisawal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malacaria_C/0/1/0/all/0/1">Christian Malacaria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">Jon M. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parker_M/0/1/0/all/0/1">Michael L. Parker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strohmayer_T/0/1/0/all/0/1">Tod E. Strohmayer</a>

We report on a spectroscopic analysis of the X-ray emission from IGR
J17062-6143 in the aftermath of its June 2020 intermediate duration Type I
X-ray burst. Using the Neutron Star Interior Composition Explorer, we started
observing the source three hours after the burst was detected with MAXI/GSC,
and monitored the source for the subsequent twelve days. We observed the tail
end of the X-ray burst cooling phase, and find that the X-ray flux is severely
depressed relative to its historic value for a three day period directly
following the burst. We interpret this intensity dip as the inner accretion
disk gradually restoring itself after being perturbed by the burst irradiation.
Superimposed on this trend we observed a $1.5$ d interval during which the
X-ray flux is sharply lower than the wider trend. This drop in flux could be
isolated to the non-thermal components in the energy spectrum, suggesting that
it may be caused by an evolving corona. Additionally, we detected a 3.4 keV
absorption line at $6.3sigma$ significance in a single $472$ s observation
while the burst emission was still bright. We tentatively identify the line as
a gravitationally redshifted absorption line from burning ashes on the stellar
surface, possibly associated with ${}^{40}{rm Ca}$ or ${}^{44}{rm Ti}$.

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