Strange quark star II: the minimal and maximal gravitational mass and the Keplerian configuration

TL;DR

This study models rapidly rotating strange quark stars using a density-dependent MIT bag model to determine their mass limits and rotational frequencies, revealing a minimum mass requirement for high rotation and aligning with observed pulsar data.

Contribution

It introduces a new approach with a density-dependent bag constant to estimate mass and rotational limits of strange quark stars, extending previous fixed-parameter models.

Findings

Minimum mass is required for high rotational frequencies.

Mass-shedding frequency is lower than fixed-bag constant models.

Keplerian frequency depends linearly on gravitational mass.

Abstract

We employ the MIT bag model with density-dependent bag constant for the equation of state (EOS) to estimate the gravitational mass and Keplerian frequency of rapidly rotating strange quark stars (SQS). In a companion paper we discuss the structural parameters of such rotating stars under the influence of strong magnetic fields. We use the LORENE library to compute the structural parameters at different rotational frequencies in the range of 1100-1300~Hz for a non-magnetized SQS. While there is no minimum limit for the mass of slowly rotating self-bound stars, by computing the maximum rotational frequency, known as the mass-shedding limit, we show that SQS must have a minimum mass to sustain high rotational frequencies. The mass-shedding frequency in our EOS model is lower than that estimated from the MIT bag model EOS with a fixed bag constant. The Keplerian frequency in our model depends linearly on the gravitational mass at the mass-shedding limit (and similarly on the minimum mass) with the slope of 0.08~${\rm kHz}/M_\odot$. We obtain mass limits aligned with the observational data for both the heaviest and the lightest observed pulsars.