dorsal/arxiv
View SchemaStrange quark star II: the minimal and maximal gravitational mass and the Keplerian configuration
| Authors | Fatemeh Kayanikhoo, Mateusz Kapusta, Miljenko Čemeljić, Wlodek Kluzniak, Leszek Zdunik |
|---|---|
| Categories | |
| ArXiv ID | 2601.09532vv1 |
| URL | https://arxiv.org/abs/2601.09532 |
| License | http://creativecommons.org/licenses/by/4.0/ |
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.
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"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.",
"arxiv_id": "2601.09532",
"authors": [
"Fatemeh Kayanikhoo",
"Mateusz Kapusta",
"Miljenko \u010cemelji\u0107",
"Wlodek Kluzniak",
"Leszek Zdunik"
],
"categories": [
"astro-ph.HE"
],
"license": "http://creativecommons.org/licenses/by/4.0/",
"title": "Strange quark star II: the minimal and maximal gravitational mass and the Keplerian configuration",
"url": "https://arxiv.org/abs/2601.09532",
"version": "v1"
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