Equilibrium sequences of non rotating and rapidly rotating crystalline color superconducting hybrid stars

Details Equilibrium sequences of non rotating and rapidly rotating crystalline color superconducting hybrid stars Equilibrium sequences of non rotating and rapidly rotating crystalline color superconducting hybrid stars

2007-10-22

arxiv.org/abs/0710.3874v2

Phys.Rev.D77:023004,2008

Astronomy and Astrophysics

Astrophysics

8 pages, 7 figures, uses RevTex

Scientific paper

10.1103/PhysRevD.77.023004

The three-flavor crystalline color-superconducting (CCS) phase of quantum chromodynamics (QCD) is a candidate phase for the ground state of cold matter at moderate densities above the density of the deconfinement phase transition. Apart from being a superfluid, the CCS phase has properties of a solid, such as a lattice structure and a shear modulus, and hence the ability to sustain multipolar deformations in gravitational equilibrium. We construct equilibrium configurations of hybrid stars composed of nuclear matter at low, and CCS quark matter at high, densities. Phase equilibrium between these phases is possible only for rather stiff equations of state of nuclear matter and large couplings in the effective Nambu--Jona-Lasinio Lagrangian describing the CCS state. We identify a new branch of stable CCS hybrid stars within a broad range of central densities which, depending on the details of the equations of state, either bifurcate from the nuclear sequence of stars when the central density exceeds that of the deconfinement phase transition or form a new family of configurations separated from the purely nuclear sequence by an instability region. The maximum masses of our non-rotating hybrid configurations are consistent with the presently available astronomical bounds. The sequences of hybrid configurations that rotate near the mass-shedding limit are found to be more compact and thus support substantially larger spins than their same mass nuclear counterparts.

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