Destruction of the star in the course of evolution of system star - intermediate-mass black hole

Main mechanism of the destruction of a star in the close vicinity of a supermassive black hole (SMBH) is the tidal disruption, when the star moves along a parabolic orbit and reaches some critical distance to the SMBH. In this paper we consider one more mechanism of the star destruction, which takes place when the low-mass star forms the close binary system with SMBH and approaches SMBH in the course of system evolution. A decisive role in this process belongs to the effect of hard radiation of SMBH due to accretion of stellar matter. The more massive is the SMBH, the larger is maximal mass of disrupted stars. For intermediate-mass black holes with masses 10 3 , 10 4 , 10 5 M ⊙ this maximal mass is about 2, 4, 5 M ⊙ .