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

中村 卓史

doi:10.24532/soken.63.2_126

Numerical calculations have been made for the formation process of axisymmetric, rotating black holes of 10M_&ofcir;. 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 &lsim; 0.3, the effect of rotation to the gravitational collapse is only to make the shape of matter oblate. For 0.3 &lsim; q &lne; 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 &lsim; 0.95. For q &lsim; 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.

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

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

この論文をさがす

説明

収録刊行物

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書き出し

問題の指摘

詳細情報詳細情報について