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Epicyclic frequencies for rotating strange quark stars: Importance of stellar oblateness

Dorota Gondek-Rosińska1,*, Włodek Kluźniak2,†, Nikolaos Stergioulas3, and Mateusz Wiśniewicz1

  • 1Institute of Astronomy, University of Zielona Góra, Lubuska 2, 65-265, Zielona Góra, Poland
  • 2Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
  • 3Department of Physics, Aristotle University of Thessaloniki, Thessaloniki 54124, Greece

  • *dorota@astro.ia.uz.zgora.pl
  • †wlodek@camk.edu.pl
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Phys. Rev. D 89, 104001 – Published 1 May, 2014

DOI: https://doi.org/10.1103/PhysRevD.89.104001

Abstract

Kilohertz quasi periodic oscillations (QPOs) can be used as a probe of the inner regions of accretion disks in compact stars and hence also of the properties of the central object. Most models of kHz QPOs involve epicyclic frequencies to explain their origin. We compute the epicyclic frequencies of nearly circular orbits around rotating strange quark stars. The MIT bag model is used to model the equation of state of quark matter, and the uniformly rotating stellar configurations are computed in full general relativity. The vertical epicyclic frequency and the related nodal precession rate of inclined orbits are very sensitive to the oblateness of the rotating star. For rotating stellar models of moderate and high-mass strange stars, the sense of the nodal precession changes at a certain rotation rate. At lower stellar rotation rates, the orbital nodal precession is prograde, as it is in the Kerr metric, while at higher rotation rates, the precession is retrograde, as it is for Maclaurin spheroids. Thus, qualitatively, the orbits around rapidly rotating strange quark stars are affected more strongly by the effects of stellar oblateness than by the effects of general relativity. We show that epicyclic and orbital frequencies calculated numerically for small mass strange stars are in very good agreement with analytical formulas for Maclaurin spheroids.

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Phys. Rev. D 89, 104001– Published 1 May, 2014
  • Received 27 December 2013

© 2014 American Physical Society

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