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Volumn 68, Issue 10, 2003, Pages

Gravitational waves from axisymmetrically oscillating neutron stars in general relativistic simulations

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Indexed keywords


EID: 85038989836     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.68.104020     Document Type: Article
Times cited : (53)

References (43)
  • 21
    • 84942855559 scopus 로고    scopus 로고
    • J. A. Font, Living Rev. Relativ. 3, 2 (2000), http://www.livingreviews.org/Articles/Volume2/2000-2font
    • (2000) Living Rev. Relativ. , vol.3 , pp. 2
    • Font, J.A.1
  • 31
    • 0000831661 scopus 로고
    • In 161819 and this paper, we adopt a formulation slightly modified from the original version presented in the following reference: M. Shibata and T. Nakamura, Phys. Rev. D 52, 5428 (1995); see also
    • (1995) Phys. Rev. D , vol.52 , pp. 5428
    • Shibata, M.1    Nakamura, T.2
  • 38
    • 85038992479 scopus 로고    scopus 로고
    • The gauge-invariant variables are computed from (Formula presented) In the linear order, (Formula presented) The linearized Einstein equation for (Formula presented) in our formulation
    • The gauge-invariant variables are computed from (Formula presented) In the linear order, (Formula presented) The linearized Einstein equation for (Formula presented) in our formulation 1619 is (Formula presented)If the Hamiltonian constraint in the linear level is satisfied, (Formula presented) Then, the solution of (Formula presented) is (Formula presented) and consequently, the gauge-invariant variables do not contain (Formula presented) However, if the Hamiltonian constraint is violated, the effects of (Formula presented) are contained in the gauge-invariant variables. In the present work, we found that its effect is small, and hence we ignore it.
  • 39
    • 85039028831 scopus 로고    scopus 로고
    • In
    • In 15, a three-dimensional simulation for an oscillating and nonrotating star which is almost the same as model S1 was performed. They computed approximate gravitational waveforms in a near zone (Formula presented) and derived the period for the fundamental quadrupole mode as (Formula presented) This value agrees with ours in (Formula presented) error.


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