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Volumn 58, Issue 2, 1998, Pages

Stability of coalescing binary stars against gravitational collapse: Hydrodynamical simulations

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Indexed keywords


EID: 0001968284     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevD.58.023002     Document Type: Article
Times cited : (37)

References (37)
  • 8
    • 4243700962 scopus 로고
    • 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 scopus 로고    scopus 로고
    • 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
  • 15
    • 0542375386 scopus 로고    scopus 로고
    • E. E. Flanagan, gr-qc/9706045
    • E. E. Flanagan, gr-qc/9706045.
  • 16
    • 26544437380 scopus 로고    scopus 로고
    • 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
  • 20
    • 33646641462 scopus 로고
    • S. Chandrasekhar, Astrophys. J. 140, 417 (1964); 142, 1519 (1965).
    • (1965) Astrophys. J. , vol.142 , pp. 1519
  • 22
    • 0542422873 scopus 로고    scopus 로고
    • R. Reith and G. Schäfer, gr-qc/9603043
    • R. Reith and G. Schäfer, gr-qc/9603043.
  • 24
    • 0039002344 scopus 로고    scopus 로고
    • 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 scopus 로고    scopus 로고
    • note
    • ij that may be erased by a gauge transformation) are included, because they appear in our gauge condition.
  • 29
    • 0542399160 scopus 로고    scopus 로고
    • 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 scopus 로고    scopus 로고
    • 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 scopus 로고    scopus 로고
    • M. Shibata, Phys. Rev. D 55, 6019 (1997); Prog. Theor. Phys. 96, 317 (1996).
    • (1996) Prog. Theor. Phys. , vol.96 , pp. 317
  • 32
    • 11944262266 scopus 로고
    • 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
  • 36
    • 85088488699 scopus 로고    scopus 로고
    • note
    • 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)].
  • 37
    • 0542422842 scopus 로고    scopus 로고
    • note
    • 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.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.