General Relativistic Collapse of Rotating Supermassive Stars

Publisher Website
Google Scholar
Abstract
Numerical calculations have been done for the formation process of axisymmetric, rotating supermassive black holes. Polytropic distribution with N = 3 is used as the initial density distribution. Calculated models are characterized by the total angular momentum (J) and the rotation law. The two types of the initial law are examined. As the effect of rotation is the strongest at the center for the differential rotation law case, the matter distribution becomes disk-like. In this case, if q = (J/M2) ≲ 0.92 an apparent horizon is formed. If q ≳ 0.92, the disk-like matter expands toward the lateral direction. For the almost rigidly rotating case, the oblate shape core is always formed because the effect of rotation at the center is not so strong as the former case. In this case if q ≲ 1.05 an apparent horizon is formed. For large q, for example q = 1.46, the central core bounces and a jet which expands mainly along the rotational axis appears. For the collapse of 109M⊙ star, the kinetic energy of the jet becomes 3.6 × 1060 ergs, which is comparable to the total energy stored in the radio lobes of the extragalactic double radio gources.

This publication has 4 references indexed in Scilit: