Formation of Intermediate Mass Black Holes in Star Burst Galaxies

(1)高密度恒星系统中的恒星爆发现象；(2)由于恒星残骸的引力相互作用而形成中等质量的S黑洞；(3)由于中等质量的中等质量黑洞的引力相互作用而成长为超大质量黑洞。这三个步骤可以划分为每个独立的过程。首先，在步骤(1)中，检查在恒星爆发现象中形成了什么残留物。由于恒星黑洞和中子星对于通常的质量函数来说太少而不能形成IMBH，因此必须考虑更平坦的质量函数。在接下来的步骤(2)中，如果我们假设恒星残留物的分布与恒星的分布相同，速度分布服从通常的高斯分布，那么由于远距离的两体引力相互作用，恒星残留物系统演化为核-晕结构。很快，三体碰撞变得有效，残留系统EVO…更倾向于高密度系统。困难的问题是，由于绝热收缩，残余系统的收缩变得如此缓慢，以至于在10Gy内不能形成IMBH。然后，在气体组分共存的情况下，考虑了气体阻力效应和超音速运动引起的激波耗散。然而，冷却效应太小，不能影响演化。由此产生的遗迹系统半径为10pc，质量为10万太阳质量。这个大小对于形成IMBH来说太大了。至于步骤(3)，我们研究了在10Gy内形成SMBH的条件。结果表明，IMBHs的累积大小为1pc，质量为100万太阳质量。如果是这样的话，(2)中形成的高密度残体系统的大小与形成SMBH所需的大小之差为4位数，这一差距很难重合。因此，在从(2)到(3)的步骤中，我们必须包括一些在本工作中没有考虑的新的物理过程。这个问题是未来研究的主题。较少

As the three points of this research are set in the followings : (1)Star burst phenomena in high dense stellar systems, (2)Formation of intermediate mass black holes(IMBH)s due to the gravitational interaction of Stellar remnants, and (3)Growth to super massive black holes(SMBHs) due to gravitational interaction of IMBHs. These three steps can be divided to each independent process.At first in the step (1), it is examined what remnants are formed in a star burst phenomenon. Since stellar black holes and neutron stars are too few to form an IMBH for a usual mass function, it is shown that a flatter mass function must be considered. In the following step (2), if we assume the distribution of stellar remnants to be the same as stellar distribution and velocity distribution to be usual Gaussian distribution, the stellar remnant system evolved to the core-halo structure due to distant two-body gravitational interaction. Soon, the three-body collisions become effective and remnant system evo … More lved to high dense system. The difficult problem is that the contraction of remnant system becomes so slow because of adiabatic contraction that the IMBH can not be formed within 10 Gy. Then, assuming the co-existence of gas-component, we included the gas drag effects and the shock dissipation due to supersonic motions. However, the cooling effect is too small to affect the evolution. The resultant remnant system is the radius 10pc and mass 100,000 solar mass. This size is too large for the formation of IMBH. As for the step (3), we examined the conditions for the formation of an SMBH within 10 Gy. It is concluded that the IMBHs must be accumulated with size 1pc and mass 1 million solar mass. If so, the difference between the size of high density remnant system formed in (2)and the necessitated size for the formation of SMBH is 4 digits, this gap is very difficult to coincide. Therefore, in the step from (2)to (3), we must include some new physical processes which are not considered in this work. This problem is the subjects of future research. Less