Equilibrium sequences of synchronized and irrotational binary systems composed of different mass stars in Newtonian gravity

Details Equilibrium sequences of synchronized and irrotational binary systems composed of different mass stars in Newtonian gravity Equilibrium sequences of synchronized and irrotational binary systems composed of different mass stars in Newtonian gravity

2001-08-06

arxiv.org/abs/astro-ph/0108086v2

Phys.Rev. D65 (2002) 044027

Astronomy and Astrophysics

Astrophysics

22 pages, 6 tables, 24 figures, revtex, Suppressed much of Sec.II, added some explanations and modified some figures, accepted

Scientific paper

10.1103/PhysRevD.65.044027

We study equilibrium sequences of close binary systems on circular orbits and composed of different mass stars with polytropic equation of state in Newtonian gravity. The solving method is a multidomain spectral method which we have recently developed. The computations are performed for both cases of synchronized and irrotational binary systems with adiabatic indices $\gamma = 3, 2.5, 2.25, 2$ and 1.8, and for three mass ratios: $M_1/M_2 =0.5, 0.2$ and 0.1. It is found that the equilibrium sequences always terminate at a mass shedding limit (appearance of a cusp on the surface of the less massive star). For synchronized binaries, this contrasts with the equal mass case, where the sequences terminate instead by a contact configuration. Regarding the turning point of the total angular momentum (or total energy) along a sequence, we find that it is difficult to get it for small mass ratios. Indeed, we do not find any turning points for $M_1/M_2 \le 0.5$ in the irrotational case. However, in the synchronized case, it becomes easier again to find one for mass ratios much smaller than $M_1/M_2 \sim 0.2$.

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