2021/12/02 by Chen Zhang, Michael Gammon, Robert B. Mann · 1 citation
Physics and Astronomy · #Pulsars and Gravitational Waves Research #Cold Atom Physics and Bose-Einstein Condensates #High-Energy Particle Collisions Research
paper · doi:10.1103/physrevd.104.123007
We explore the stellar structure and radial stability of charged quark stars composed of interacting quark matter in three classes of commonly used charge models. We adopt a general parametrization of interacting quark matter equation of state that includes the corrections from perturbative QCD, color superconductivity, and the strange quark mass into one parameter \ensuremathλ, or one dimensionless parameter \ensuremathλ=\ensuremathλ2/(4Beff) after being rescaled with the effective bag constant Beff. We find that increasing charge tends to increase the mass and radius profiles, and enlarges the separation size in mass between the maximum mass point and the point where zero eigenfrequencies \ensuremathω02=0 of the fundamental radial oscillation mode occur. The sign of the separation in central density depends on the charge model; this separation also has a dependence on \ensuremathλ such that increasing \ensuremathλ (which can occur for either large color superconductivity or small strange quark mass) tends to decrease this separation size for the first and third classes of charge models monotonically. Moreover, for the second and third classes of charge models, we manage to numerically and analytically identify a new kind of stellar structure with a zero central pressure but with a finite radius and mass. All the calculations and analysis are performed in a general dimensionless rescaling approach so that the results are independent of explicit values of dimensional parameters.