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Volumn 69, Issue 10, 2004, Pages

General relativistic hydrodynamics with viscosity: Contraction, catastrophic collapse, and disk formation in hypermassive neutron stars

Author keywords

[No Author keywords available]

Indexed keywords


EID: 3042784522     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.69.104030     Document Type: Article
Times cited : (137)

References (90)
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    • A similar approach was suggested in 18 to simulate r-mode evolution and was successfully applied in 19
    • A similar approach was suggested in 18 to simulate r-mode evolution and was successfully applied in 19.
  • 39
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    • C.W. Misner, K.S. Thorne, and J.A. Wheeler, Gravitation (Freeman, New York, 1973), p. 566.
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    • L.D. Landau and E.M. Lifshitz, Fluid Mechanics (Butterworth-Heinemann, London, 1987).
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    • H.O. Kreiss and J. Oliger, Methods for the Approximate Solution of Time Dependent Problems, GARP Publication Series No. 10 (World Meteorological Organization, Geneva, 1973)
    • H.O. Kreiss and J. Oliger, Methods for the Approximate Solution of Time Dependent Problems, GARP Publication Series No. 10 (World Meteorological Organization, Geneva, 1973)
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    • N.Ó. Murchadha and J.W. York, Jr., Phys. Rev. D 10, 2345 (1974)
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    • R.M. Wald, General Relativity (University of Chicago Press, Chicago, 1984), p. 297.
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  • 70
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    • In paper I, star A was labeled “C” and star B was labeled “D.”
    • In paper I, star A was labeled “C” and star B was labeled “D.”
  • 77
    • 85039602198 scopus 로고    scopus 로고
    • What appears to be a drift in (Formula presented) due to numerical error becomes visible toward the end of the simulation. This makes the extrapolated value of (Formula presented) less reliable than the values of (Formula presented) and (Formula presented)
    • What appears to be a drift in (Formula presented) due to numerical error becomes visible toward the end of the simulation. This makes the extrapolated value of (Formula presented) less reliable than the values of (Formula presented) and (Formula presented)
  • 79
    • 0042740426 scopus 로고    scopus 로고
    • Disks can form from the collapse of uniformly rotating polytropes near the mass-shedding limit, provided (Formula presented) [see M. Shibata and S.L. Shapiro, Astrophys. J. 577, 904 (2002)].
    • (2002) Astrophys. J. , vol.577 , pp. 904
    • Shibata, M.1    Shapiro, S.L.2
  • 89
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    • D. Mihalas and B. Weibel-Mihalas, Foundations of Radiation Hydrodynamics (Dover, Mineola, NY, 1999)
    • D. Mihalas and B. Weibel-Mihalas, Foundations of Radiation Hydrodynamics (Dover, Mineola, NY, 1999)


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.