Slowly rotating proto strange stars in Quark mass density- and temperature- dependent model

Abstract

Employing the Quark Mass Denisity- and temperature- dependent model and the Hartle's method, We have studied the slowly rotating strange star with uniform angular velocity. The mass-radius relation, the moment of inertia and the frame dragging for different frequencies are given. We found that we cannot use the strange star to solve the challenges of Stella and Vietri for the horizontal branch oscillations and the moment of inertia $I_{45}/(M/M_s)>2.3$. Furthermore, we extended the Hartle's method to study the differential rotating strange star and found that the differential rotation is an effective way to get massive strange star.

arXiv commentLatex file, 13 figures, accepted for publication in Inter. J. Mod. Phys. A

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• Warm asymmetric quark matter and proto-quark stars within the confined-isospin-density-dependent mass model
• Quark deconfinement phase transition for improved quark mass density-dependent model
• Spin Down of Rotating Compact Magnetized Strange Stars in General Relativity
• Slowly rotating neutron stars and hadronic stars in chiral SU(3) quark mean field model