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We have performed magnetohydrodynamic simulations in general relativity ofbinary neutron star and binary black hole-neutron star mergers, as well as themagnetorotational collapse of supermassive stars. In many cases the outcome isa spinnng black hole (BH) immersed in a magnetized disk, with a jet emanatingfrom the poles of the BH. While their formation scenarios differ and their BHmasses, as well as their disk masses, densities, and magnetic field strengths,vary by orders of magnitude, these features conspire to generate jet Poyntingluminosities that all lie in the same, narrow range of $\sim 10^{52\pm1}~{\rmerg ~s^{-1}}$. A similar result applies to their BH accretion rates upon jetlaunch, which is $\sim 0.1-10~{\rm M_{\odot}~s^{-1}}$. We provide a simplemodel that explains these unanticipated findings. Interestingly, theseluminosities reside in the same narrow range characterizing the observedluminosity distributions of over 400 short and long GRBs with distancesinferred from spectroscopic redshifts or host galaxies. This result, togetherwith the GRB lifetimes predicted by the model, supports the belief that acompact binary merger is the progenitor of an SGRB, while a massive, stellarmagnetorotational collapse is the progenitor of an LGRB.

Black holes, disks and jets following binary mergers and stellar collapse: The narrow range of EM luminosities and accretion rates