메뉴 건너뛰기




Volumn 61, Issue 6, 2000, Pages

Simulation of merging binary neutron stars in full general relativity: [formula presented] case

Author keywords

[No Author keywords available]

Indexed keywords


EID: 85037214482     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.61.064001     Document Type: Article
Times cited : (35)

References (62)
  • 2
    • 85037189989 scopus 로고    scopus 로고
    • For example, S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars (Wiley Interscience, New York, 1983)
    • For example, S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars (Wiley Interscience, New York, 1983).
  • 14
    • 85037201241 scopus 로고    scopus 로고
    • For example, 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, and references therein
    • For example, 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, and references therein.
  • 18
    • 85037239222 scopus 로고    scopus 로고
    • astro-ph/9904038
    • P. Meszaros, astro-ph/9904038.
    • Meszaros, P.1
  • 34
    • 0004273913 scopus 로고
    • C. R. Evans, L. S. Finn, D. W. Hobill
    • T. Nakamura and K. Oohara, in Frontiers in Numerical Relativity, edited by C. R. Evans, L. S. Finn, and D. W. Hobill (Cambridge University Press, Cambridge, England, 1989), p. 254.
    • (1989) Frontiers in Numerical Relativity , pp. 254
    • Nakamura, T.1    Oohara, K.2
  • 35
    • 85037203564 scopus 로고    scopus 로고
    • K. Oohara and T. Nakamura, in Relativistic Gravitation and Gravitational Radiation, edited by J.-P. Lasota and J.-A. Marck (Cambridge University Press, Cambridge, England, 1997), p. 309
    • K. Oohara and T. Nakamura, in Relativistic Gravitation and Gravitational Radiation, edited by J.-P. Lasota and J.-A. Marck (Cambridge University Press, Cambridge, England, 1997), p. 309.
  • 43
    • 85037208290 scopus 로고    scopus 로고
    • K. Uryū and Y. Eriguchi (unpublished)
    • K. Uryū and Y. Eriguchi (unpublished).
  • 47
    • 85037182627 scopus 로고    scopus 로고
    • The equation for the Hamiltonian constraint is written in the form (Formula presented) where (Formula presented) and (Formula presented) are the Laplacian with respect to (Formula presented) and a function of (Formula presented) (Formula presented) (Formula presented) (Formula presented) P and (Formula presented) We define a function (Formula presented) for measuring the violation of the Hamiltonian constraint. We have found that (Formula presented) is typically less than (Formula presented) for a region in which (Formula presented) is larger than (Formula presented) For the less dense region, however, (Formula presented) often becomes (Formula presented) because such a low density region is not well resolved in our finite differencing scheme for the hydrodynamic equations
    • The equation for the Hamiltonian constraint is written in the form (Formula presented) where (Formula presented) and (Formula presented) are the Laplacian with respect to (Formula presented) and a function of (Formula presented) (Formula presented) (Formula presented) (Formula presented) P and (Formula presented) We define a function (Formula presented) for measuring the violation of the Hamiltonian constraint. We have found that (Formula presented) is typically less than (Formula presented) for a region in which (Formula presented) is larger than (Formula presented) For the less dense region, however, (Formula presented) often becomes (Formula presented) because such a low density region is not well resolved in our finite differencing scheme for the hydrodynamic equations.
  • 48
    • 85037255991 scopus 로고    scopus 로고
    • The rest mass is conserved because of no mass ejection. The angular momentum decreases by 5–10 % in the whole evolution, and the total amount of the decrease roughly agrees with the angular momentum emission in gravitational waves within (Formula presented) error [see Eq. (4.2)]
    • The rest mass is conserved because of no mass ejection. The angular momentum decreases by 5–10 % in the whole evolution, and the total amount of the decrease roughly agrees with the angular momentum emission in gravitational waves within (Formula presented) error [see Eq. (4.2)].
  • 50
    • 85037178114 scopus 로고    scopus 로고
    • The definition of differential rotation depends on the coordinate condition. Strictly speaking, we have found that the new massive neutron star is differentially rotating in our present gauge, and the rotation law found in this paper could change slightly if it is defined in the stationary axisymmetric gauge used in
    • The definition of differential rotation depends on the coordinate condition. Strictly speaking, we have found that the new massive neutron star is differentially rotating in our present gauge, and the rotation law found in this paper could change slightly if it is defined in the stationary axisymmetric gauge used in 4.
  • 51
    • 85037199275 scopus 로고    scopus 로고
    • Note that we recompute the constraint equations whenever we modify the initial quasiequilibrium configurations
    • Note that we recompute the constraint equations whenever we modify the initial quasiequilibrium configurations.
  • 53
    • 0542371321 scopus 로고    scopus 로고
    • For example, M. Shibata, Phys. Rev. D 58, 024012 (1998), and references therein.
    • (1998) Phys. Rev. D , vol.58 , pp. 24012
    • Shibata, M.1
  • 54
    • 85037223759 scopus 로고    scopus 로고
    • Actually, it is possible to construct differentially rotating neutron stars of such a large mass, which are dynamically (but not always secularly) stable against gravitational collapse and bar mode deformation 5;M. Shibata, T. W. Baumgarte, and S. L. Shapiro (in preparation).
    • Shibata, M.1    Baumgarte, T.W.2    Shapiro, S.L.3
  • 56
    • 85037245345 scopus 로고    scopus 로고
    • The new, massive neutron stars may be secularly unstable to becoming a black hole on a long time scale even if the effect of gravitational radiation is small. The reason is that they are differentially rotating and supramassive, which implies if we take into account the effects of viscosity or magnetic fields, angular momentum will be transported outward or dissipated, and eventually they may become unstable to gravitational collapse. See also
    • The new, massive neutron stars may be secularly unstable to becoming a black hole on a long time scale even if the effect of gravitational radiation is small. The reason is that they are differentially rotating and supramassive, which implies if we take into account the effects of viscosity or magnetic fields, angular momentum will be transported outward or dissipated, and eventually they may become unstable to gravitational collapse. See also 5.
  • 59
    • 85037177781 scopus 로고    scopus 로고
    • If the time duration is fairly long, we may be able to observe a peak around the oscillation frequency in the Fourier spectrum of gravitational waves as pointed out in
    • If the time duration is fairly long, we may be able to observe a peak around the oscillation frequency in the Fourier spectrum of gravitational waves as pointed out in 15. On the other hand, we will not find the peak if the time duration is short. Thus, we may say that the amplitude of the peak in the Fourier space also provides important information.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.