Dynamical determination of the innermost stable circular orbit of binary neutron stars

Physical Review Letters

Volumn 92, Issue 14, 2004, Pages

  Marronetti, Pedro ^a   Duez, Matthew D ^a   Shapiro, Stuart L ^a,c   Baumgarte, Thomas W ^a,b  

^a University of Illinois at Urbana Champaign   (United States)

^b BOWDOIN COLLEGE   (United States)

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

Author keywords

[No Author keywords available]

Indexed keywords

APPROXIMATION THEORY; BOUNDARY CONDITIONS; COALESCENCE; COMPUTER SIMULATION; DATA REDUCTION; ERROR ANALYSIS; FREQUENCIES; GRAVITATIONAL EFFECTS; HYDRODYNAMICS; STABILITY;

ANGULAR FREQUENCIES; ANGULAR MOMENTUM; BLACK HOLES; DATA SETS;

ASTROPHYSICS;

EID: 2542487761     PISSN: 00319007     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevLett.92.141101     Document Type: Article

References (29)

1. T.W. Baumgarte and S. L. Shapiro, Phys. Rep. 376, 41 (2003).
2. M. Shibata and K. Uryū, Phys. Rev. D 61, 064001 (2000); M. Shibata and K. Uryū, Prog. Theor. Phys. 107, 265 (2002).
3. M. Shibata and K. Uryū, Phys. Rev. D 61, 064001 (2000); M. Shibata and K. Uryū, Prog. Theor. Phys. 107, 265 (2002).
4. A. Ori and K. S. Thorne, Phys. Rev. D 62, 124022 (2000); A. Buonanno and T. Damour, Phys. Rev. D 62, 064015 (2000).
5. A. Ori and K. S. Thorne, Phys. Rev. D 62, 124022 (2000); A. Buonanno and T. Damour, Phys. Rev. D 62, 064015 (2000).
6. M. D. Duez, T.W. Baumgarte, S. L. Shapiro, M. Shibata, and K. Uryū, Phys. Rev. D 65, 024016 (2001).
7. T.W. Baumgarte, in Astrophysical Sources of Gravitational Radiation, edited by J. M. Centrella (AIP, New York, 2001).
8. F. A. Rasio and S. L. Shapiro, Classical Quantum Gravity 16, R1 (1999).
9. J. L. Friedman, J. R. Ipser, and R. D. Sorkin, Astrophys. J. 325, 722 (1988).
10. T. W. Baumgarte, G. B. Cook, M. A. Scheel, S. L. Shapiro, and S. A. Teukolsky, Phys. Rev. D 57, 6181 (1998).
11. Approximating the stars as ellipsoids, it has been shown that the dynamical orbital instability occurs quite close to the secular instability for irrotational binaries in both Newtonian and first-order post-Newtonian theory [D. Lai, F. A. Rasio, and S. L. Shapiro, Astrophys. J. Suppl. 88, 205 (1993)].
12. P. Marronetti and S. L. Shapiro, Phys. Rev. D 68, 104024 (2003).
13. For simplicity, in the reminder of the paper we will refer to the zero circulation models as irrotational. See [10] for comparisons between these models and irrotational binaries.
14. C.S. Kochanek, Astrophys. J. 398, 234 (1992); L. Bildsten and C. Cutler, Astrophys. J. 400, 175 (1992).
15. C.S. Kochanek, Astrophys. J. 398, 234 (1992); L. Bildsten and C. Cutler, Astrophys. J. 400, 175 (1992).
16. K. Uryū, M. Shibata, and Y. Eriguchi, Phys. Rev. D 62, 104015 (2000).
17. E. Gourgoulhon, P. Grandclément, K. Taniguchi, J.-A. Marck, and S. Bonazzola, Phys. Rev. D 63, 064029 (2001).
18. Gamma;. For scaling with k, see Ref. [8].
19. M. D. Duez, P. Marronetti, S.L. Shapiro, and T.W. Baumgarte, Phys. Rev. D 67, 024004 (2003).
20. M. Shibata and T. Nakamura, Phys. Rev. D 52, 5428 (1995); T.W. Baumgarte and S. L. Shapiro, Phys. Rev. D 59, 024007 (1999).
21. M. Shibata and T. Nakamura, Phys. Rev. D 52, 5428 (1995); T.W. Baumgarte and S. L. Shapiro, Phys. Rev. D 59, 024007 (1999).
22. F.D. Swesty, E.Y. Wang, and A.C. Calder, Astrophys. J. 541, 937 (2000).
23. The time coordinate has been transformed into fractions of the initial orbital period. Note that the periods differ for binaries at different separation.
24. J. C. Lombardi, F. A. Rasio, and S. L. Shapiro, Phys. Rev. D 56, 3416 (1997).
25. The total angular momentum like the gravitational mass is not strictly conserved due to the emission of gravitational waves. However, the loss rate of angular momentum for a typical orbit at these separations is of the order of 1% to 2%. Deviations exceeding these values therefore indicate numerical error.
26. 2 norm of the constraint residuals. The details of these plots as well as the normalizations used here can be found in [16], In this Letter, the momentum constraint curve shows the average of the three spatial components.
27. M. Miller, gr-qc/0305024.
28. M. Miller and W.M. Suen, gr-qc/0301112; M. Miller, P. Gressman, and W. M. Suen, gr-qc/0312030.
29. Small amounts of spurious radiation present in the initial data are radiated away, leaving M and J nearly unchanged.