  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.
