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0001465920
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Note, however, that collapse of a rotating cluster of collisionless matter is studied in the following reference: A. M. Abrahams, G. B. Cook, S. L. Shapiro and S. A. Teukolsky, Phys. Rev. D49 (1994), 5153.
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L. S. Finn and C. R. Evans, Astrophys. J. 351 (1990), 588. R. Mönchmeyer, G. Schäfer, E. Müller and R. Kates, Astron. Astrophys. 246 (1991), 417. S. Bonazzola and J.-A. Marck, Astron. Astrophys. 267 (1993), 623. S. Yamada and K. Sato, Astrophys. J. 450 (1995), 245. T. Zwerger and E. Müller, Astron. Astrophys. 332 (1997), 209. M. Rampp, E. Müller and M. Ruffert, Astron. Astrophys. 332 (1998), 969.
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85037768676
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But, for a special class of gauge conditions with appropriate prescriptions, it is still possible to preserve the accuracy and stability without artificial viscosity (e.g., D. Garfinkle, personal communication)
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But, for a special class of gauge conditions with appropriate prescriptions, it is still possible to preserve the accuracy and stability without artificial viscosity (e.g., D. Garfinkle, personal communication).
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26
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85037784095
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gr-qc/9908012
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M. Alcubierre, S. Brandt, B. Brügmann, D. Holz, E. Seidel, R. Takahashi and J. Thornburg, gr-qc/9908012.
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Thornburg, J.7
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31
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85037779654
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note
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1/Γ/ρ =constant holds during the evolution in the absence of the artificial viscosity.
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34
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0000872666
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For example, H. Komatsu, Y. Eriguchi and I. Hachisu, Mon. Not. R. Astron. Soc. 237 (1989), 355. G. Cook, S. L. Shapiro and S. A. Teukolsky, Astrophys. J. 398 (1992), 203. S. Bonazzola, E. Gourgoulhon, M. Salgado and J.-A. Marck, Astron. Astrophys. 278 (1993), 421.
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11944271977
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Cook, G.1
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36
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0001349368
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For example, H. Komatsu, Y. Eriguchi and I. Hachisu, Mon. Not. R. Astron. Soc. 237 (1989), 355. G. Cook, S. L. Shapiro and S. A. Teukolsky, Astrophys. J. 398 (1992), 203. S. Bonazzola, E. Gourgoulhon, M. Salgado and J.-A. Marck, Astron. Astrophys. 278 (1993), 421.
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39
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85037779367
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-1/2 is smaller than 3.6, a black hole could be formed for the case in which the gravitational binding energy is sufficiently large initially. Hence, the value 3.6 is not an absolute threshold, even for q = 0, although it could be a good guideline
-
-1/2 is smaller than 3.6, a black hole could be formed for the case in which the gravitational binding energy is sufficiently large initially. Hence, the value 3.6 is not an absolute threshold, even for q = 0, although it could be a good guideline.
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40
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85037766046
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We reached this conclusion because convergence was not well achieved when Ν was increased
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We reached this conclusion because convergence was not well achieved when Ν was increased.
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41
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85037760560
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max denotes the maximum density at t = 0
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max denotes the maximum density at t = 0.
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44
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85037768926
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g, could maintain a stable orbit
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g, could maintain a stable orbit.
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45
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0003513781
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Wiley Interscience, New York, chapter 12
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For example, S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars (Wiley Interscience, New York, 1983), chapter 12.
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(1983)
Black Holes, White Dwarfs, and Neutron Stars
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Shapiro, S.L.1
Teukolsky, S.A.2
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