Physics
Scientific paper
Apr 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007acasn..48..121w&link_type=abstract
Acta Astronomica Sinica, vol. 48, no. 2, p. 121-129
Physics
Physical Data And Processes: Black Hole Physics, Stars: Evolution, Stars: Mass-Loss, Stars: Population Ii
Scientific paper
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 formation of black hole binaries is a very complex and difficult subject. It focuses on the masses of black holes in black hole binaries and their distribution only. According to the results of Fryer's two-dimensional core-collapse supernova simulations (TS) it is found that the relation between the explosion energy and the binding energy dominates the mass of remnant of primary star evolved in such a binary system as mentioned above. And then, on the one hand the binding energy lies on the mass of helium core strongly. The computing shows that the binding energy contributed by hydrogen shell is less than 10% of whole. On the other hand the explosion energy can be regarded as the function of the mass of helium core approximately. Thus it is found that the remnant mass may relate to the mass of helium core directly. It fits 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, a theoretical distribution of the initial mass of black holes in binaries is gotten. At present, there are 17 candidates of black hole binaries in the data of observation and the distribution of the mass of these candidates shows that there is a peak around ~7Msun. However, there is a difference between the shape of the theoretical distribution and the shape of observation. The theoretical distributional peak appears around ~5Msun. But then, according to the thought of Podsiadlowski, Rappaport & Han 2003 (PRH), the observational distribution can not show the distribution of initial mass of black holes maybe. There is a mechanism of the masses of black holes increasing. Through the analysis, there is a probability increasing the peak value from ~5Msun to ~7Msun. The results support the thought of PRH somewhat.
Han Zhan-Wen
Meng Xiang-Cun
Wu Baofeng
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