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Volumn 61, Issue 4, 2000, Pages

Stability and collapse of rapidly rotating, supramassive neutron stars: 3D simulations in general relativity

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Indexed keywords


EID: 16644379019     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.61.044012     Document Type: Article
Times cited : (95)

References (43)
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    • The Binary Black Hole Grand Challenge Alliance, R. Gomez, Phys. Rev. Lett. 80, 3915 (1998).
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    • The Binary Black Hole Grand Challenge Alliance, A. M. Abrahams, Phys. Rev. Lett. 80, 1812 (1998).
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    • Throughout this paper, we use (Formula presented) as the central rest mass density of equilibrium stars (initial data for our computation) and (Formula presented) as the central rest mass density of dynamically evolved stars (i.e., the latter changes during the evolution)
    • Throughout this paper, we use (Formula presented) as the central rest mass density of equilibrium stars (initial data for our computation) and (Formula presented) as the central rest mass density of dynamically evolved stars (i.e., the latter changes during the evolution).
  • 39
    • 85037193405 scopus 로고    scopus 로고
    • Note that we recompute the constraint equations whenever we modify the initial equilibrium configurations (e.g., by depleting the pressure or by modifying the initial density profile)
    • Note that we recompute the constraint equations whenever we modify the initial equilibrium configurations (e.g., by depleting the pressure or by modifying the initial density profile).


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