STELLAR TIDAL DISRUPTION EVENTS BY DIRECT-COLLAPSE BLACK HOLES

We analyze the early growth stage of direct-collapse black holes (DCBHs) with similar to 10(5) M-circle dot, which are formed by collapse of supermassive stars in atomic-cooling halos at z greater than or similar to 10. A nuclear accretion disk around a newborn DCBH is gravitationally unstable and fragments into clumps with a few x 10 M-circle dot at similar to 0.01-0.1 pc from the center. Such clumps evolve into massive Population III stars with a few x 10-10(2) M-circle dot via successive gas accretion, and a nuclear star cluster is formed. Radiative and mechanical feedback from an inner slim disk and the star cluster will significantly reduce the gas accretion rate onto the DCBH within similar to 10(6) yr. Some of the nuclear stars can be scattered onto the loss cone orbits also within less than or similar to 106 yr and tidally disrupted by the central DCBH. The jet luminosity powered by such tidal disruption events can be L-j greater than or similar to 10(50) erg s(-1). The prompt emission will be observed in X-ray bands with a peak duration of delta t(obs) similar to 10(5-6)(1 + z) s followed by a tail proportional to t(obs) (-5/3), which can be detectable by Swift BAT and eROSITA even from z similar to 20. Follow-up observations of the radio afterglows with, e.g., eVLA and the host halos with James Webb Space Telescope could probe the earliest active galactic nucleus feedback from DCBHs.