Rotating compact strange stars
D. Gondek-Rosinska, T. Bulik, J. L. Zdunik, E. Gourgoulhon, S. Ray, J., Dey, M. Dey

TL;DR
This paper models rotating strange stars using a QCD-based equation of state, revealing their unique properties, high rotation frequencies, and differences from neutron stars, with implications for their stability and maximum mass limits.
Contribution
It provides the first detailed numerical models of rotating strange stars based on a QCD-inspired EOS, highlighting their distinct physical characteristics and rotational behaviors.
Findings
Strange stars have higher surface redshift than MIT bag model stars.
Maximum rotation frequencies of strange stars exceed those of neutron stars.
Supramassive strange stars spin up as they lose angular momentum before collapse.
Abstract
We compute numerical models of uniformly rotating strange stars (SS) in general relativity for the recently proposed QCD-based equation of state (EOS) of strange quark matter (Dey et al. 1998). Static models based on this EOS are characterised by a larger surface redshift than strange stars within the MIT bag model. The frequencies of the fastest rotating configurations described by Dey model are much higher than these for neutron stars (NS) and for the simplest SS MIT bag model. We determine a number of physical parameters for such stars and compare them with those obtained for NS. We construct constant baryon mass equilibrium sequences both normal and supramassive. Similarly to the NS a supramassive SS, prior to collapse to a black hole, spins up as it loses angular momentum. We find the upper limits on maximal masses and maximal frequencies of the rotating configurations. We show…
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Taxonomy
TopicsPulsars and Gravitational Waves Research · Stellar, planetary, and galactic studies · Astronomy and Astrophysical Research
