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Published December 15, 1994 | Submitted + Published
Journal Article Open

Disk collapse in general relativity


The radial collapse of a homogeneous disk of collisionless particles can be solved analytically in Newtonian gravitation. To solve the problem in general relativity, however, requires the full machinery of numerical relativity. The collapse of a disk is the simplest problem that exhibits the two most significant and challenging features of strong-field gravitation: black hole formation and gravitational wave generation. We carry out dynamical calculations of several different relativistic disk systems. We explore the growth of ring instabilities in equilibrium disks, and how they are suppressed by sufficient velocity dispersion. We calculate waveforms from oscillating disks, and from disks that undergo gravitational collapse to black holes. Studies of disk collapse to black holes should also be useful for developing new techniques for numerical relativity, such as apparent horizon boundary conditions for black hole spacetimes.

Additional Information

© 1994 American Physical Society. {Received 25 May 1994) This work was supported by National Science Foundation Grant No. AST 91-19475 and No. PHY 90-07834 and by Grand Challenge Grant No. NSF PHY 93-18152/ASC 93-18152 (ARPA supplemented). Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.

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Submitted - 9405060.pdf

Published - PhysRevD.50.7282.pdf


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August 20, 2023
August 20, 2023