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- W2148924596 abstract "General relativistic quasiequilibrium states of black hole-neutron star binaries are computed in the moving-puncture framework. We propose three conditions for determining the quasiequilibrium states and compare the numerical results with those obtained in the excision framework. We find that the results obtained in the moving-puncture framework agree with those in the excision framework and with those in the third post-Newtonian approximation for the cases that (i) the mass ratio of the binary is close to unity irrespective of the orbital separation, and (ii) the orbital separation is large enough ($m_0Omega alt 0.02$ where $m_0$ and $Omega$ are the total mass and the orbital angular velocity, respectively) irrespective of the mass ratio. For $m_0 Omega agt 0.03$, both of the results in the moving-puncture and excision frameworks deviate, more or less, from those in the third post-Newtonian approximation. Thus the numerical results do not provide a quasicircular state, rather they seem to have a nonnegligible eccentricity of order 0.01--0.1. We show by numerical simulation that a method in the moving-puncture framework can provide approximately quasicircular states in which the eccentricity is by a factor of $sim 2$ smaller than those in quasiequilibrium given by other approaches." @default.
- W2148924596 created "2016-06-24" @default.
- W2148924596 creator A5005410621 @default.
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- W2148924596 date "2009-06-12" @default.
- W2148924596 modified "2023-10-18" @default.
- W2148924596 title "Quasiequilibrium states of black hole-neutron star binaries in the moving-puncture framework" @default.
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- W2148924596 doi "https://doi.org/10.1103/physrevd.79.124018" @default.
- W2148924596 hasPublicationYear "2009" @default.
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