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

TL;DR

This paper investigates slowly rotating and differentially rotating strange stars using a quark mass density- and temperature-dependent model, analyzing their mass-radius relation, moment of inertia, and frame dragging effects.

Contribution

It extends Hartle's method to differential rotation and explores the properties of strange stars within a density- and temperature-dependent quark model.

Findings

Cannot use strange stars to explain certain stellar oscillation challenges.

Differential rotation effectively increases the maximum mass of strange stars.

Mass-radius relations and frame dragging effects are characterized for various rotation frequencies.

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.