Figure 1: Mass gap , diquark gap and isospin chemical potential as a function of the baryon chemical potential for different values of the antineutrino chemical potential . Solutions obey -equilibrium and charge neutrality conditions. | |
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Figure 2: Pressure vs. baryon chemical potential ( left panel) and energy density ( right panel) for different values of the antineutrino chemical potential . Due to antineutrino trapping the onset of superconductivity in quark matter is shifted to higher energy densities and the equation of state becomes harder. | |
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Figure 3: Quark star configurations for different antineutrino chemical potentials MeV. The total mass M in solar masses ( in the text) is shown as a function of the radius R ( left panel) and of the central number density n_{q} in units of the nuclear saturation density n_{0} ( right panel). Asterisks denote two different sets of configurations (A, B, f) and (A' ,B' ,f') with a fixed total baryon number of the set. | |
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Figure 4: Quark star configurations with diquark condensation as a function of the central number density n_{q} in units of the nuclear number density n_{0}. The mass defect for the transition from initial configurations with MeV to a final configuration with at constant total baryon number is shown. | |
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Figure 5: Mass defect and corresponding energy release due to antineutrino untrapping as a function of the mass of the final state . The shaded region is defined by the estimates for the upper and lower limits of the antineutrino chemical potential in the initial state MeV (dashed-dotted line) and MeV (dashed line), respectively. | |
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