Radial oscillation spectra of an anisotropic strange quark star model of Cen X-3 are computed for three anisotropy prescriptions and differ by up to 40 percent between models.
Strange star equation of state fits the refined mass measurement of 12 pulsars and predicts their radii
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abstract
There are three categories of stars whose masses have been found accurately in recent times: (1) two for which Shapiro delay is used which is possible due to GR light bending as the partner is heavy : PSR J1614-2230 and PSR J1903+0327 (2) six eclipsing stars for which numerical Roche Lobe geometry is used and (3) 3 stars for which spectroscopic methods are used and in fact for these three the mass and radii both are estimated. Motivated by large color (N_c) expansion using a modified Richardson potential, along with density dependent quark masses thereby allowing chiral symmetry restoration, we get compact strange stars fitting all the observed masses.
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On Modeling Anisotropic Quark Stars: The Role of Anisotropy in Radial Oscillation Spectra
Radial oscillation spectra of an anisotropic strange quark star model of Cen X-3 are computed for three anisotropy prescriptions and differ by up to 40 percent between models.