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There are three categories of stars whose masses have been found accuratelyin recent times: (1) two for which Shapiro delay is used which is possible dueto 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 threethe mass and radii both are estimated. Motivated by large color (N_c) expansionusing a modified Richardson potential, along with density dependent quarkmasses thereby allowing chiral symmetry restoration, we get compact strangestars fitting all the observed masses.

Strange star equation of state fits the refined mass measurement of 12 pulsars and predicts their radii