All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{GE_NEU_0862.ps} \end{figure}$ Figure 1: Mass gap $\phi$ , diquark gap $\Delta$ and isospin chemical potential $\mu _{\rm I}$ as a function of the baryon chemical potential $\mu _{\rm B}$ for different values of the antineutrino chemical potential $\mu_{\bar \nu_{\rm e}}$ . Solutions obey $\beta$ -equilibrium and charge neutrality conditions.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{EoS_NEU_0862.ps} \end{figure}$ Figure 2: Pressure vs. baryon chemical potential ( left panel) and energy density ( right panel) for different values of the antineutrino chemical potential $\mu_{\bar \nu_{\rm e}}$ . 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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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{smzoom_0862.ps} \end{figure}$ Figure 3: Quark star configurations for different antineutrino chemical potentials $\mu_{\bar \nu_{\rm e}}=0,~100,~150$ MeV. The total mass M in solar masses ( $M_{{\rm sun}}\equiv M_\odot$ 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 n₀ ( 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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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Effect_0862.ps} \end{figure}$ 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 n₀. The mass defect for the transition from initial configurations with $\mu_{\bar \nu_{\rm e}}=100,~150$ MeV to a final configuration with $\mu_{\bar \nu_{\rm e}}=0$ at constant total baryon number is shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{DeltaM_0862.eps} \end{figure}$ Figure 5: Mass defect $\Delta M$ and corresponding energy release $\Delta E$ due to antineutrino untrapping as a function of the mass of the final state $M_{\rm f}$ . The shaded region is defined by the estimates for the upper and lower limits of the antineutrino chemical potential in the initial state $\mu_{\bar \nu_{\rm e}}=150$ MeV (dashed-dotted line) and $\mu_{\bar \nu_{\rm e}}=100$ MeV (dashed line), respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{GE_NEU_0862.ps} \end{figure}$	Figure 1: Mass gap $\phi$ , diquark gap $\Delta$ and isospin chemical potential $\mu _{\rm I}$ as a function of the baryon chemical potential $\mu _{\rm B}$ for different values of the antineutrino chemical potential $\mu_{\bar \nu_{\rm e}}$ . Solutions obey $\beta$ -equilibrium and charge neutrality conditions.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{EoS_NEU_0862.ps} \end{figure}$	Figure 2: Pressure vs. baryon chemical potential ( left panel) and energy density ( right panel) for different values of the antineutrino chemical potential $\mu_{\bar \nu_{\rm e}}$ . 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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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Effect_0862.ps} \end{figure}$	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 n₀. The mass defect for the transition from initial configurations with $\mu_{\bar \nu_{\rm e}}=100,~150$ MeV to a final configuration with $\mu_{\bar \nu_{\rm e}}=0$ at constant total baryon number is shown.
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