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Strange star equation of state fits the refined mass measurement of 12 pulsars and predicts their radii
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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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Cited by 2 Pith papers
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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.
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Karmarkar-Tolman Embedded Charged Anisotropic Stars in f(R) Gravity
Charged anisotropic star models with a Karmarkar-Tolman metric are constructed in three f(R) gravity models and tested graphically for energy conditions and stability.
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