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We show results from the radiation hydrodynamics (RHD) simulations of tidaldisruption of a star on a parabolic orbit by a supermassive black hole (SMBH)based on a three-dimensional smoothed particle hydrodynamics code withradiative transfer. We find that such a tidally disrupted star fragment andform clumps soon after its tidal disruption. The fragmentation results from theendothermic processes of ionization and dissociation that reduce the gaspressure, leading to local gravitational collapse. Radiative cooling is lesseffective because the stellar debris is still highly optically thick in such anearly time. Our simulations reveal that a solar-type star with a stellardensity profile of n=3 disrupted by a 10^6 solar mass black hole produces$\sim20$ clumps of masses in the range of 0.1 to 12 Jupiter masses. The massfallback rate decays with time, with pronounced spikes from early to late time.The spikes provide evidence for the clumps of the returning debris, while theclumps on the unbound debris can be potentially freely-floating planets andbrown dwarfs. This ionization and dissociation induced fragmentation on atidally disrupted star are a promising candidate mechanism to form low-massstars to planets around an SMBH.

Ionization and dissociation induced fragmentation of a tidally disrupted star into planets around a supermassive black hole