Properties of general relativistic, irrotational binary neutron stars in close quasiequilibrium orbits: Polytropic equations of state

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 62, Issue 10, 2000, Pages 1-15

  Uryu, Koji ^a   Shibata, Masaru ^b,c   Eriguchi, Yoshiharu ^d  

^a SISSA   (Italy)

^b UNIVERSITY OF ILLINOIS AT URBANA CHAMPAIGN   (United States)

^c OSAKA UNIVERSITY   (Japan)

^d UNIVERSITY OF TOKYO   (Japan)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 3242734055     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevD.62.104015     Document Type: Article

References (69)

1. C. Cutler et al., Phys. Rev. Lett. 70, 1984 (1993); K. S. Thorne, in Proceeding of Snowmass 95 Summer Study on Particle and Nuclear Astrophysics and Cosmology, edited by E. W. Kolb and R. Peccei (World Scientific, Singapore, 1995), p. 398.
2. C. Cutler et al., Phys. Rev. Lett. 70, 1984 (1993); K. S. Thorne, in Proceeding of Snowmass 95 Summer Study on Particle and Nuclear Astrophysics and Cosmology, edited by E. W. Kolb and R. Peccei (World Scientific, Singapore, 1995), p. 398.
3. A. Abramovici et al., Science 256, 325 (1992); C. Bradaschia et al., Nucl. Instrum. Methods Phys. Res. A 289, 518 (1990); J. Hough, in Proceedings of the Sixth Marcel Grossmann Meeting, edited by H. Sato and T. Nakamura (World Scientific, Singapore, 1992), p. 192; K. Kuroda et al., in Proceedings of the International Conference on Gravitational Waves: Sources and Detectors, edited by I. Ciufolini and F. Fidecard (World Scientific, Singapore, 1997), p. 100.
4. A. Abramovici et al., Science 256, 325 (1992); C. Bradaschia et al., Nucl. Instrum. Methods Phys. Res. A 289, 518 (1990); J. Hough, in Proceedings of the Sixth Marcel Grossmann Meeting, edited by H. Sato and T. Nakamura (World Scientific, Singapore, 1992), p. 192; K. Kuroda et al., in Proceedings of the International Conference on Gravitational Waves: Sources and Detectors, edited by I. Ciufolini and F. Fidecard (World Scientific, Singapore, 1997), p. 100.
5. A. Abramovici et al., Science 256, 325 (1992); C. Bradaschia et al., Nucl. Instrum. Methods Phys. Res. A 289, 518 (1990); J. Hough, in Proceedings of the Sixth Marcel Grossmann Meeting, edited by H. Sato and T. Nakamura (World Scientific, Singapore, 1992), p. 192; K. Kuroda et al., in Proceedings of the International Conference on Gravitational Waves: Sources and Detectors, edited by I. Ciufolini and F. Fidecard (World Scientific, Singapore, 1997), p. 100.
6. A. Abramovici et al., Science 256, 325 (1992); C. Bradaschia et al., Nucl. Instrum. Methods Phys. Res. A 289, 518 (1990); J. Hough, in Proceedings of the Sixth Marcel Grossmann Meeting, edited by H. Sato and T. Nakamura (World Scientific, Singapore, 1992), p. 192; K. Kuroda et al., in Proceedings of the International Conference on Gravitational Waves: Sources and Detectors, edited by I. Ciufolini and F. Fidecard (World Scientific, Singapore, 1997), p. 100.
7. E.g., T. Piran, in Unsolved Problems in Astrophysics, edited by J. N. Bahcall and J. P. Ostriker (Princeton University Press, Princteon, NJ, 1997), p. 343.
8. L.-X. Li and B. Paczynski, Astrophys. J. Lett. 507, L59 (1998).
9. E.g., L. Blanchet, in Relativistic Gravitation and Gravitational Radiation, edited by J.-P. Lasota and J.-A. Marck (Cambridge University Press, Cambridge, England, 1997), p. 33; Prog. Theor. Phys. Suppl. 136, 146 (1999); C. M. Will, ibid. 136, 158 (1999).
10. E.g., L. Blanchet, in Relativistic Gravitation and Gravitational Radiation, edited by J.-P. Lasota and J.-A. Marck (Cambridge University Press, Cambridge, England, 1997), p. 33; Prog. Theor. Phys. Suppl. 136, 146 (1999); C. M. Will, ibid. 136, 158 (1999).
11. E.g., L. Blanchet, in Relativistic Gravitation and Gravitational Radiation, edited by J.-P. Lasota and J.-A. Marck (Cambridge University Press, Cambridge, England, 1997), p. 33; Prog. Theor. Phys. Suppl. 136, 146 (1999); C. M. Will, ibid. 136, 158 (1999).
12. X. Zhuge, J. M. Centrella, and S. L. W. McMillan, Phys. Rev. D 50, 6247 (1994); 54, 7261 (1996).
13. X. Zhuge, J. M. Centrella, and S. L. W. McMillan, Phys. Rev. D 50, 6247 (1994); 54, 7261 (1996).
14. Note however that if a dual recycling technique for a narrow band detector is available, it may be still possible to detect gravitational waves of high-frequency beyond ∼1 kHz [1].
15. K. Oohara and T. Nakamura, in Relativistic Gravitation and Gravitational Radiation (Ref. [5]), p. 309; Prog. Theor. Phys. Suppl. 136, 270 (1999).
16. K. Oohara and T. Nakamura, in Relativistic Gravitation and Gravitational Radiation (Ref. [5]), p. 309; Prog. Theor. Phys. Suppl. 136, 270 (1999).
17. J. A. Font, M. Miller, W.-M. Suen, and M. Tobias, Phys. Rev. D 61, 044011 (2000); W.-M. Suen, Prog. Theor. Phys. Suppl. 136, 251 (1999).
18. J. A. Font, M. Miller, W.-M. Suen, and M. Tobias, Phys. Rev. D 61, 044011 (2000); W.-M. Suen, Prog. Theor. Phys. Suppl. 136, 251 (1999).
19. M. Shibata, Prog. Theor. Phys. 101, 251 (1999); 101, 1199 (1999); Phys. Rev. D 60, 104052 (1999).
20. M. Shibata, Prog. Theor. Phys. 101, 251 (1999); 101, 1199 (1999); Phys. Rev. D 60, 104052 (1999).
21. M. Shibata, Prog. Theor. Phys. 101, 251 (1999); 101, 1199 (1999); Phys. Rev. D 60, 104052 (1999).
22. M. Shibata and K. Uryū, Phys. Rev. D 61, 064001 (2000).
23. W. Landry and S. A. Teukolsky, gr-qc/9912004 (1999).
24. C. S. Kochanek, Astrophys. J. 398, 234 (1992); L. Bildsten and C. Cutler, ibid. 400, 175 (1992).
25. C. S. Kochanek, Astrophys. J. 398, 234 (1992); L. Bildsten and C. Cutler, ibid. 400, 175 (1992).
26. S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, Phys. Rev. D 56, 7740 (1997); H. Asada, ibid. 57, 7292 (1998).
27. S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, Phys. Rev. D 56, 7740 (1997); H. Asada, ibid. 57, 7292 (1998).
28. M. Shibata, Phys. Rev. D 58, 024012 (1998).
29. S. A. Teukolsky, Astrophys. J. 504, 442 (1998).
30. For example, H. Heiselberg and M. Hjorth-Jensen, Phys. Rep. 328, 237 (2000).
31. D. Lai, F. A. Rasio, and S. L. Shapiro, Astrophys. J., Suppl. 88, 205 (1993); Astrophys. J. 420, 811 (1994).
32. D. Lai, F. A. Rasio, and S. L. Shapiro, Astrophys. J., Suppl. 88, 205 (1993); Astrophys. J. 420, 811 (1994).
33. J. C. Lombardi, Jr., F. A. Rasio, and S. L. Shapiro, Phys. Rev. D 56, 3416 (1997).
34. E.g., S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs and Neutron Stars (Wiley, New York, 1983).
35. 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).
36. 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).
37. S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998); S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, Phys. Rev. Lett. 82, 892 (1999).
38. S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998); S. Bonazzola, E. Gourgoulhon, and J.-A. Marck, Phys. Rev. Lett. 82, 892 (1999).
39. P. Marronetti, G. J. Mathews, and J. R. Wilson, in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998); Phys. Rev. D 60, 087301 (1999).
40. P. Marronetti, G. J. Mathews, and J. R. Wilson, in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998); Phys. Rev. D 60, 087301 (1999).
41. K. Uryū and Y. Eriguchi, Phys. Rev. D 61, 124023 (2000).
42. 0 where υ denotes characteristic magnitude of the orbital velocity: See, e.g., H. Asada and M. Shibata, Phys. Rev. D 54, 4944 (1996).
43. F. Usui, K. Uryū, and Y. Eriguchi, Phys. Rev. D 61, 024038 (2000).
44. K. Uryū and Y. Eriguchi, Mon. Not. R. Astron. Soc. 296, L1 (1998); Astrophys. J., Suppl. 118, 563 (1998); Mon. Not. R. Astron. Soc. 303, 329 (1999); in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998).
45. K. Uryū and Y. Eriguchi, Mon. Not. R. Astron. Soc. 296, L1 (1998); Astrophys. J., Suppl. 118, 563 (1998); Mon. Not. R. Astron. Soc. 303, 329 (1999); in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998).
46. K. Uryū and Y. Eriguchi, Mon. Not. R. Astron. Soc. 296, L1 (1998); Astrophys. J., Suppl. 118, 563 (1998); Mon. Not. R. Astron. Soc. 303, 329 (1999); in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998).
47. K. Uryū and Y. Eriguchi, Mon. Not. R. Astron. Soc. 296, L1 (1998); Astrophys. J., Suppl. 118, 563 (1998); Mon. Not. R. Astron. Soc. 303, 329 (1999); in the Proceedings of 19th Texas Symposium on Relativistic Astrophysics: Texas in Paris, Paris, France (1998).
48. max have been shown to give accurate results.
49. We changed d̂ by steps of 0.125 typically to construct a solution sequence and by steps of 0.0625 near to the minima of J̄ and M̄ when they appear on the sequence.
50. Here, we refer to the general relativistic orbital instability as being that determined only by general relativistic gravity between two bodies and independent of any hydrodynamic effects and finite-size effects, such as the orbital instability for a test particle orbiting near to a black hole. In this definition, the ISCO determined by the general relativistic instability should never depend on (M/R)∞ because of the strong equivalence principle.
51. G. B. Cook, Phys. Rev. D 50, 5025 (1994).
52. T. W. Baumgarte, Phys. Rev. D 62, 024018 (2000).
53. L. E. Kidder, C. M. Will, and A. G. Wiseman, Class. Quantum Grav. 9, L125 (1992); Phys. Rev. D 47, 3281 (1993).
54. L. E. Kidder, C. M. Will, and A. G. Wiseman, Class. Quantum Grav. 9, L125 (1992); Phys. Rev. D 47, 3281 (1993).
55. T. Damour, B. R. Iyer, and B. S. Sathyaprakash, Phys. Rev. D 57, 885 (1998).
56. A. Buonanno and T. Damour, Phys. Rev. D 59, 084006 (1999).
57. E. E. Flanagan, Phys. Rev. D 58, 124030 (1998); K. S. Thorne, ibid. 58, 124031 (1998).
58. E. E. Flanagan, Phys. Rev. D 58, 124030 (1998); K. S. Thorne, ibid. 58, 124031 (1998).
59. 2 is expected to decrease by ∼10%.
60. T. W. Baumgarte, S. L. Shapiro, and M. Shibata, Astrophys. J. Lett. 528, L29 (2000); M. Shibata, T. W. Baumgarte, and S. L. Shapiro, Astrophys. J. (to be published), astro-ph/0005378.
61. T. W. Baumgarte, S. L. Shapiro, and M. Shibata, Astrophys. J. Lett. 528, L29 (2000); M. Shibata, T. W. Baumgarte, and S. L. Shapiro, Astrophys. J. (to be published), astro-ph/0005378.
62. T. W. Baumgarte, G. B. Cook, M. A. Scheel, S. L. Shapiro, and S. A. Teukolsky, Phys. Rev. D 57, 6181 (1998); 57, 7299 (1998).
63. T. W. Baumgarte, G. B. Cook, M. A. Scheel, S. L. Shapiro, and S. A. Teukolsky, Phys. Rev. D 57, 6181 (1998); 57, 7299 (1998).
64. The hydrodynamic interaction could be an important mechanism for outward angular momentum transportation in particular for the case when spiral arms are formed in the outer region of a merger object and an ellipsoidal object is formed in the inner region. However, recent results of numerical simulations for the merger of irrotational binaries [11] show that such structures are not formed significantly, which indicates that the timescale of the transportation could not be short enough to increase the specific angular momentum of a certain fraction of fluid elements.
65. BH.]
66. E.g., K. Oohara, T. Nakamura, and M. Shibata, Prog. Theor. Phys. Suppl. 128, 183 (1997).
67. R. Sorkin, Astrophys. J. 249, 254 (1981); J. R. Ipser and G. Horowitz, ibid. 232, 863 (1979); J. Katz, Mon. Not. R. Astron. Soc. 183, 765 (1978).
68. R. Sorkin, Astrophys. J. 249, 254 (1981); J. R. Ipser and G. Horowitz, ibid. 232, 863 (1979); J. Katz, Mon. Not. R. Astron. Soc. 183, 765 (1978).
69. R. Sorkin, Astrophys. J. 249, 254 (1981); J. R. Ipser and G. Horowitz, ibid. 232, 863 (1979); J. Katz, Mon. Not. R. Astron. Soc. 183, 765 (1978).