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Showing 1 to 6 of 6 for “"color superconductivity"”.
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Gapless color superconductivity
… thesis, we propose and investigate the "Gapless Color-Flavor Locked" (gCFL) phase, a possible new phase of dense and cold quark matter. At high enough densities, quarks interact with each other and form pairs similarly to electrons in superconductors. This phenomenon in the case of quark matter …
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Two key questions about color superconductivity
We pose two key questions about color superconductivity: What are the effects of the large strange quark mass, and what are the observable consequences of color superconductivity? Motivated by the first question, we study crystalline color superconductivity. We adapt the Nambu-Gor'kov formalism to …
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Color superconducting phase of cold dense quark matter
We investigate color superconducting phases of cold quark matter at densities relevant for the interiors of compact stars. At these densities, electrically neutral and weak-equilibrated quark matter can have unequal numbers of up, down, and strange quarks. The QCD interaction favors Cooper pairs …
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Study of the properties of dilute Fermi gases in the strongly interacting regime
… relation to the spin polarized alkali gases and color superconductivity of the quark matter. Unlike the two component fluids, zero potential range limit cannot be reached without causing collapse of the system. We also study the scaling behavior of the three-body system. We calculate the …
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Cold, dense quark matter
… realization of quark-hadron continuity in the color-flavor locked (CFL) quark superfluid, and the implications of these issues to quark matter equations of state, and thus to neutron star structure including the mass-radius (M-R) relation. In Chapter 1, we present a general overview of quark …
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Probing the phases of cold ultra-dense matter using neutron star physics
… and low temperatures is predicted to be in a “color superconducting” phase. At high enough densities, quark matter is in the Color-Flavor-Locked: CFL) phase, but the possible phases of matter at intermediate densities are unknown. Since the density at the core of a neutron star can be as high …