Equilibrium sequences of irrotational binary polytropic stars : The case of double polytropic stars

Abstract

Solutions to equilibrium sequences of irrotational binary polytropic stars in Newtonian gravity are expanded in a power of $\epsilon =a_0/R$, where R and $a_0$ are the orbital separation of the binary system and the radius of each star for $R=\infty$. For each order of $\epsilon$, we should solve ordinary differential equations for arbitrary polytropic indices n. We show solutions for polytropic indices n= 0.5, 1, 1.5 and 2 up to ${\epsilon }^6$ orders. Our semi-analytic solutions can be used to check the validity of numerical solutions.

59 pages including 15 tables and 13 figures, revtex, accepted to Phys. Rev. D

References in corpus (8)

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• A new numerical method for constructing quasi-equilibrium sequences of irrotational binary neutron stars in general relativity
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• Quasiequilibrium black hole-neutron star binaries in general relativity
• Various features of quasiequilibrium sequences of binary neutron stars in general relativity
• Post-Newtonian SPH calculations of binary neutron star coalescence. II. Binary mass ratio, equation of state, and spin dependence
• Non-conformally flat initial data for binary compact objects
• Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. II. Newtonian limits
• Equilibrium sequences of synchronized and irrotational binary systems composed of different mass stars in Newtonian gravity
• Toroidal figures of equilibrium from a 2nd-order accurate, accelerated SCF-method with subgrid approach