Kavli Affiliate: Erin Kara
| First 5 Authors: Zijian Zhang, Lars Lund Thomsen, Lixin Dai, Christopher S. Reynolds, Javier A. García
| Summary:
It has been recently discovered that a few super-Eddington sources undergoing
black hole super-Eddington accretion exhibit X-ray reflection signatures. In
such new systems, one expects that the coronal X-ray emissions are mainly
reflected by optically thick super-Eddington winds instead of thin disks. In
this paper, we conduct a series of general relativistic ray-tracing and Monte
Carlo radiative transfer simulations to model the X-ray reflection signatures,
especially the characteristic Fe K$alpha$ line, produced from super-Eddington
accretion flows around non-spinning black holes. In particular, we allow the
photons emitted by a lamppost corona to be reflected multiple times in a
cone-like funnel surrounded by fast winds. We find that the Fe K$alpha$ line
profile most sensitively depends on the wind kinematics, while its exact shape
also depends on the funnel open angle and corona height. Furthermore, very
interestingly, we find that the Fe K$alpha$ line can have a prominent
double-peak profile in certain parameter spaces even with a face-on
orientation. Moreover, we compare the Fe K$alpha$ line profiles produced from
super-Eddington and thin disks and show that such lines can provide important
insights into the understanding of black hole systems undergoing
super-Eddington accretion.
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