-
7
-
-
0000345345
-
-
gr-qc/9709026
-
T. W. Baumgarte, G. B. Cook, M. A. Scheel, S. L. Shapiro, and S. A. Teukolsky, Phys. Rev. D 57, 7299 (1998), gr-qc/9709026.
-
(1998)
Phys. Rev. D
, vol.57
, pp. 7299
-
-
Baumgarte, T.W.1
Cook, G.B.2
Scheel, M.A.3
Shapiro, S.L.4
Teukolsky, S.A.5
-
8
-
-
4243700962
-
-
J. R. Wilson and G. J. Mathews, Phys. Rev. Lett. 75, 4161 (1995); J. R. Wilson, G. J. Mathews and P. Marronetti, Phys. Rev. D 54, 1317 (1996); gr-qc/9710140 (WMM).
-
(1995)
Phys. Rev. Lett.
, vol.75
, pp. 4161
-
-
Wilson, J.R.1
Mathews, G.J.2
-
9
-
-
0000537359
-
-
gr-qc/9710140 (WMM)
-
J. R. Wilson and G. J. Mathews, Phys. Rev. Lett. 75, 4161 (1995); J. R. Wilson, G. J. Mathews and P. Marronetti, Phys. Rev. D 54, 1317 (1996); gr-qc/9710140 (WMM).
-
(1996)
Phys. Rev. D
, vol.54
, pp. 1317
-
-
Wilson, J.R.1
Mathews, G.J.2
Marronetti, P.3
-
10
-
-
0004424255
-
-
D. Lai, F. A. Rasio and S. L. Shapiro, Astrophys. J., Suppl. Ser. 88, 205 (1993).
-
(1993)
Astrophys. J., Suppl. Ser.
, vol.88
, pp. 205
-
-
Lai, D.1
Rasio, F.A.2
Shapiro, S.L.3
-
15
-
-
0542375386
-
-
E. E. Flanagan, gr-qc/9706045
-
E. E. Flanagan, gr-qc/9706045.
-
-
-
-
16
-
-
26544437380
-
-
to be published, gr-qc/9706057
-
K. S. Thorne, Phys. Rev. D. (to be published), gr-qc/9706057.
-
Phys. Rev. D.
-
-
Thorne, K.S.1
-
17
-
-
4243482123
-
-
T. W. Baumgarte, S. L. Shapiro, G. B. Cook, M. A. Scheel, and S. A. Teukolsky, Phys. Rev. Lett. 79, 1182 (1997);
-
(1997)
Phys. Rev. Lett.
, vol.79
, pp. 1182
-
-
Baumgarte, T.W.1
Shapiro, S.L.2
Cook, G.B.3
Scheel, M.A.4
Teukolsky, S.A.5
-
18
-
-
0000201414
-
-
T. W. Baumgarte, S. L. Shapiro, G. B. Cook, M. A. Scheel, and S. A. Teukolsky, Phys. Rev. D 57, 6181 (1998).
-
(1998)
Phys. Rev. D
, vol.57
, pp. 6181
-
-
Baumgarte, T.W.1
Shapiro, S.L.2
Cook, G.B.3
Scheel, M.A.4
Teukolsky, S.A.5
-
20
-
-
33646641462
-
-
S. Chandrasekhar, Astrophys. J. 140, 417 (1964); 142, 1519 (1965).
-
(1965)
Astrophys. J.
, vol.142
, pp. 1519
-
-
-
22
-
-
0542422873
-
-
R. Reith and G. Schäfer, gr-qc/9603043
-
R. Reith and G. Schäfer, gr-qc/9603043.
-
-
-
-
23
-
-
0030504799
-
-
H. Asada, M. Shibata, and T. Futamase, Prog. Theor. Phys. 96, 81 (1996); H. Asada and M. Shibata, Phys. Rev. D 54, 4944 (1996).
-
(1996)
Prog. Theor. Phys.
, vol.96
, pp. 81
-
-
Asada, H.1
Shibata, M.2
Futamase, T.3
-
24
-
-
0039002344
-
-
H. Asada, M. Shibata, and T. Futamase, Prog. Theor. Phys. 96, 81 (1996); H. Asada and M. Shibata, Phys. Rev. D 54, 4944 (1996).
-
(1996)
Phys. Rev. D
, vol.54
, pp. 4944
-
-
Asada, H.1
Shibata, M.2
-
26
-
-
0542399192
-
-
note
-
ij that may be erased by a gauge transformation) are included, because they appear in our gauge condition.
-
-
-
-
28
-
-
0003513781
-
-
Wiley, New York, Chap. 6
-
S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars (Wiley, New York, 1983), Chap. 6.
-
(1983)
Black Holes, White Dwarfs, and Neutron Stars
-
-
Shapiro, S.L.1
Teukolsky, S.A.2
-
29
-
-
0542399160
-
-
note
-
Note that for the case where the star expands, we stopped the computation when the surface of the star reached the outer boundary of numerical grid. Since the star is gravitationally bound, the star ultimately has to recontract and collapse.
-
-
-
-
30
-
-
0000000886
-
-
M. Shibata, Phys. Rev. D 55, 6019 (1997); Prog. Theor. Phys. 96, 317 (1996).
-
(1997)
Phys. Rev. D
, vol.55
, pp. 6019
-
-
Shibata, M.1
-
31
-
-
0030505215
-
-
M. Shibata, Phys. Rev. D 55, 6019 (1997); Prog. Theor. Phys. 96, 317 (1996).
-
(1996)
Prog. Theor. Phys.
, vol.96
, pp. 317
-
-
-
32
-
-
11944262266
-
-
C. S. Kochanek, Astrophys. J. 398, 234 (1992); L. Bildsten and C. Cutler, ibid. 400, 175 (1992).
-
(1992)
Astrophys. J.
, vol.398
, pp. 234
-
-
Kochanek, C.S.1
-
35
-
-
0001627910
-
-
see also talk at GRG 15, India, 1997
-
S. Bonazzola, E. Gourgoulhon and J.-A. Marck, Phys. Rev. D 56, 7740 (1997); see also talk at GRG 15, India, 1997.
-
(1997)
Phys. Rev. D
, vol.56
, pp. 7740
-
-
Bonazzola, S.1
Gourgoulhon, E.2
Marck, J.-A.3
-
36
-
-
85088488699
-
-
note
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j,i=0 (M. Shibata, preprint OU-TAP 73, unpublished). Here, however, Γε≥1, so that Eq. (4.2) may be regarded as an approximate irrotational condition [cf. Eq. (2.9)].
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37
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0542422842
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note
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For stiffer equations of state with higher Γ, the bulk of the mass would suffer greater tidal distortion at the same separation. Our near-equilibrium spherical approximation would require larger orbital separations, and hence more numerical resolution, to be as reliable in these cases.
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