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

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

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pthph..65.1876n&link_type=abstract

Progress of Theoretical Physics, Vol. 65, No. 6, pp. 1876-1890

Physics

71

Scientific paper

Numerical calculations have been made for the formation process ofaxisymmetric, rotating black holes of 10M&sun;. The initialdensity of a star is about 3 × 1013 g/cm^3. Numericalresults are classified mainly by q which corresponds to |a|/M in a Kerr black hole. For q ≲ 0.3, theeffect of rotation to the gravitational collapse is only to make theshape of matter oblate. For 0.3 ≲ q≤0.95, although thedistribution of matter is disk-like, a ring-like peak of properdensity appears. This ring is inside the apparent horizon, which isalways formed in the case 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.

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