On the Physical Nature of the Source of Ultraluminous X-ray Pulsations

TL;DR

This paper proposes a novel black hole-based explanation for the ultraluminous X-ray pulsations of M82X-2, suggesting it is a spinning intermediate mass black hole emitting X-ray pulsations due to rotational energy, with detailed energetics and orbital parameters.

Contribution

It introduces a microscopic black hole theory to explain ultraluminous X-ray pulsations, providing a new model for the source's nature and detailed physical parameters.

Findings

M82X-2 is modeled as a spinning intermediate mass black hole.

The black hole releases 99.6% of its energy as X-ray pulsations.

Derived orbital parameters and spin-up rate consistent with observations.

Abstract

To reconcile the observed unusual high luminosity of NuSTAR X-ray pulsations from M82X-2 with the most extreme violation of the Eddington limit, and in view that the persistent X-ray radiation from M82X-2 almost precludes the possibility of common pulsars, we tackle the problem by the implications of {\em microscopic theory of black hole} (MTBH). The preceding developments of MTBH are proved to be quite fruitful for the physics of ultra-high energy (UHE) cosmic-rays. Namely, replacing a central singularity by the infrastructures inside event horizon, subject to certain rules, MTBH explains the origin of ZeV-neutrinos which are of vital interest for the source of UHE-particles. The M82X-2 is assumed to be a spinning intermediate mass black hole resided in final stage of growth. As a corollary, the thermal blackbody X-ray emission arisen due to the rotational kinetic energy of black hole escapes from event horizon through the vista to outside world that detected as ultraluminous X-ray pulsations. The M82X-2 indeed releases $\sim 99.6\%$ of its pulsed radiative energy predominantly in the X-ray bandpass $0.3-30$ keV. We derive a pulse profile and give a quantitative account of energetics and orbital parameters of the semi-detached X-ray binary containing a primary accretor M82X-2 of inferred mass $M\simeq 138.5-226\,M_{\odot}$ and secondary massive, $M_{2}> 48.3- 64.9\,M_{\odot}$, O/B-type donor star with radius of $R> 22.1- 25.7\,R_{\odot}$, respectively. We compute the torque added to M82X-2 per unit mass of accreted matter which yields the measured spin-up rate.