The Formation Of The Black Hole Binary

A binary system which contains a massive primary star goes through a phase of common envelope and the less massive companion spirals-in thereafter. If the common envelope is ejected completely and the system avoids merging, it is possible to form a black hole binary. So far, to observe the black hole binaries is the only way to find out the stellar-mass black holes effectively. It is important somewhat to study the formation of black hole binaries. The thesis will introduce the basic knowledge about the black hole binaries (such as the mechanism of supernova).The formation of black hole binaries is a very complex and difficult subject. In this paper we study about the masses of black holes in black hole binaries and their distribution only. From the results of Fryer's two-dimensional core-collapse supernova simulations (TS) we fit a quantitative relation between the mass of helium cores of black hole progenitors and the mass of black holes collapsed. The relation can be used more conveniently than TS's because of its simple form. Especially, it can be used in binary systems expediently. Combining with the PPE code we get a theoretical distribution of the mass of black holes in binaries. We attempt to give somewhat reasonable explanation for the observational distribution.