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Stellar mass black holes (SMBHs), forming by the core collapse of verymassive, rapidly rotating stars, are expected to exhibit a high densityaccretion disk around them developed from the spinning mantle of the collapsingstar. 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 weestablish a correlation between the spin and mass of SMBHs at their formationstage. Our work shows that spinning BHs are more massive than non-spinning BHsfor a given M_dot. However, slowly spinning BHs can turn out to be more massivethan spinning BHs if M_dot at their formation stage was higher compared tofaster spinning BHs.

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