# The crust of rotating strange quark stars

@article{Zdunik2001TheCO,
title={The crust of rotating strange quark stars},
author={Julian Leszek Zdunik and Paweł Haensel and E. Gourgoulhon},
journal={Astronomy and Astrophysics},
year={2001},
volume={372},
pages={535-543}
}
• Published 6 April 2001
• Physics, Geology
• Astronomy and Astrophysics
Calculations of the properties of rotating strange stars with crusts are performed within the framework of general relativity. We employ an equation of state (EOS) of strange quark matter based on the MIT Bag Model with massive strange quarks and lowest order QCD interactions. The crust is described by the BPS equation of state. A signicant increase of the stellar radius is found close to the Keplerian (mass-shedding limit) conguration. This leads to the disappearance of the gap between the…

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## References

SHOWING 1-10 OF 28 REFERENCES
Thermal structure of accreting neutron stars and strange stars
• Physics
• 1990
Steady-state models of accreting neutron stars and strange stars are presented, and their properties as a function of accretion rate are analyzed. The models have steady-state envelopes, with
Rapidly Rotating Neutron Stars in General Relativity: Realistic Equations of State
• Physics
• 1993
We construct equilibrium sequences of rotating neutron stars in general relativity. We compare results for fourteen nuclear matter equations of state. We determine a number of important physical
Innermost stable circular orbits around relativistic rotating stars
• Physics
• 1998
We investigate the innermost stable circular orbit (ISCO) of a test particle moving on the equatorial plane around rotating relativistic stars such as neutron stars. First, we derive approximate
Physics of Neutron Star Interiors
• Physics
• 2001
Microscopic Theory of the Nuclear Equation of State and Neutron Star Structure.- Superfluidity in Neutron Star Matter.- Relativistic Superfluid Models for Rotating Neutron Stars.- The Tensor Virial
Bar mode instability in relativistic rotating stars: A post-Newtonian treatment
• Physics
• 1997
We construct analytic models of incompressible, uniformly rotating stars in post-Newtonian (PN) gravity and evaluate their stability against nonaxisymmetric bar modes. We model the PN configurations
Is SAX J1808.4-3658 a Strange Star ?
• Physics
• 1999
The possibility of strange stars is one of the most important issues in the study of compact objects. Here we use the observations of the newly discovered millisecond x-ray pulsar SAX J1808.4-3658 to
Observational evidence for strange matter in compact objects from the x-ray burster 4U 1820-30
We present systematic calculations of the mass-radius (MR) relation of a neutron star (NS) using a large variety of modern equations of state (EOS) of dense matter. The role of strangeness on the EOS
Is GRO J1744-28 a strange star?
The unusual hard x-ray burster GRO J1744-28 recently discovered by the Compton Gamma-Ray Observatory can be modeled as a strange star with a dipolar magnetic field of </=10(11) gauss, and the burst energy, duration, interval, and spectrum derived from such a model are consistent with the observations.
Gamma-ray bursts and afterglows from rotating strange starsand neutron stars
• Physics
• 1998
We here discuss a new model of $\gamma$-ray bursts (GRBs) based on differentially rotating strange stars. Strange stars in this model and differentially rotating neutron stars in the
Numerical approach for high precision 3D relativistic star models
• Physics
• 1998
A multidomain spectral method for computing very high precision three-dimensional stellar models is presented. The boundary of each domain is chosen in order to coincide with a physical discontinuity