General Relativistic Collapse of Axially Symmetric Stars Leading to the Formation of Rotating Black Holes

概要

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Numerical calculations have been made for the formation process of axisymmetric, rotating black holes of 10M_⦿. The initial density of a star is about 3×10^<13>g/cm^3. Numerical results are classified mainly by q which corresponds to |a|/M in a Kerr black hole. For q ≲ 0.3, the effect of rotation to the gravitational collapse is only to make the shape of matter oblate. For 0.3 ≲ q ⪇ 0.95, although the distribution of matter is disk-like, a ring-like peak of proper density appears. This ring is inside the apparent horizon, which is always formed in the case of q ≲ 0.95. For q ≲ 0.95, no apparent horizon is formed. The distribution of matter shows a central disk plus an expanding ring. It is found that electromagnetic-like field in the [(2+1)+1]-formalism plays an important role in a formation of a rotating black hole. Local conservation of angular momentum is checked. Accuracy of constraint equations is also shown to see the truncation error in the numerical calculations.
素粒子論グループ素粒子研究編集部の論文
1981-05-20