We calculate the structure of accretion disks around Kerr black holes for accretion rates = 0.001-10 M☉ s-1. Such high- disks are plausible candidates for the central engine of gamma-ray bursts. Our disk model is fully relativistic and accurately treats the microphysics of the accreting matter: neutrino emissivity, opacity, electron degeneracy, and nuclear composition. The neutrino-cooled disk forms above a critical accretion rate ign that depends on the black hole spin. The disk has an "ignition" radius rign where neutrino flux rises dramatically, cooling becomes efficient, and the proton-to-nucleon ratio Ye drops. Other characteristic radii are rα, where most of α-particles are disintegrated, rν, where the disk becomes ν-opaque, and rtr, where neutrinos get trapped and advected into the black hole. We find rα, rign, rν, and rtr and show their dependence on . We discuss the qualitative picture of accretion and present sample numerical models of the disk structure. All neutrino-cooled disks regulate themselves to a characteristic state such that: (1) electrons are mildly degenerate, (2) Ye ~ 0.1, and (3) neutrons dominate the pressure in the disk.
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