Establishing a relation between mass and spin of stellar mass black holes

TL;DR

This paper explores the relationship between the mass and spin of stellar mass black holes formed from collapsing stars, linking neutrino luminosity to these properties and the accretion rate.

Contribution

It establishes a novel correlation between black hole spin and mass at formation, considering neutrino cooled accretion disks and their physics.

Findings

Spinning black holes tend to be more massive than non-spinning ones at the same accretion rate.

Slowly spinning black holes can be more massive than faster spinning ones if their initial accretion rates were higher.

The study provides insights into black hole formation conditions based on neutrino emission and accretion dynamics.

Abstract

Stellar mass black holes (SMBHs), forming by the core collapse of very massive, rapidly rotating stars, are expected to exhibit a high density accretion disk around them developed from the spinning mantle of the collapsing star. A wide class of such disks, due to their high density and temperature, are effective emitters of neutrinos and hence called neutrino cooled disks. Tracking the physics relating the observed (neutrino) luminosity to the mass, spin of black holes (BHs) and the accretion rate (M_dot) of such disks, here we establish a correlation between the spin and mass of SMBHs at their formation stage. Our work shows that spinning BHs are more massive than non-spinning BHs for a given M_dot. However, slowly spinning BHs can turn out to be more massive than spinning BHs if M_dot at their formation stage was higher compared to faster spinning BHs.