Single color and single flavor color superconductivity

Alford, Mark; Bowers, Jeffrey A.; Cheyne, Jack M.; Cowan, G. A.

doi:10.1103/physrevd.67.054018

Cited by 105 publications

(112 citation statements)

References 54 publications

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“…It is likely that cross-flavor (blue-up and bluedown) pairing is suppressed by a large mismatch between the Fermi surfaces of the up and down quarks. Pairing is expected in the color 6 S and flavor 3 S channel, which is same-flavor and same-color pairing, so is not affected by the flavor asymmetry (Alford et al 2003). However, the pairing in this channel vanishes in the chiral limit, when the mass of blue quarks vanishes.…”

Section: Modeling Cooling Processesmentioning

confidence: 99%

“…Because the 2SC pairing pattern breaks the SU(3) color symmetry, one of the quark colors (say, the blue color) is not involved in that pairing. The strength and the flavor content of pairing among blue quarks is model dependent (Alford et al 2003;Schmitt et al 2003;Schmitt 2005;Aguilera et al 2005Aguilera et al , 2006Aguilera 2007). It is likely that cross-flavor (blue-up and bluedown) pairing is suppressed by a large mismatch between the Fermi surfaces of the up and down quarks.…”

Section: Modeling Cooling Processesmentioning

confidence: 99%

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Rapid cooling of Cassiopeia A as a phase transition in dense QCD

Sedrakian

2013

A&A

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We present a model of the compact star in Cassiopea A that accounts for its unusually fast cooling behavior. This feature is interpreted as an enhancement in the neutrino emission triggered by a transition from a fully gapped, two-flavor, color-superconducting phase to a crystalline phase or an alternative gapless, color-superconducting phase. By fine-tuning a single parameter -the temperature of this transition -a specific cooling scenario can be selected that fits the Cas A data. Such a scenario requires a massive M ∼ 2 M star and is, therefore, distinctive from models invoking canonical 1.4 M mass star with nucleonic pairing alone.

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Section: Modeling Cooling Processesmentioning

confidence: 99%

Section: Modeling Cooling Processesmentioning

confidence: 99%

Rapid cooling of Cassiopeia A as a phase transition in dense QCD

Sedrakian

2013

A&A

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“…We expect β 1 since the secondary pairing is by definition weaker than the primary pairing. For the Cγ 0 γ 5 secondary channel in a single-gluon-based NJL interaction, β ∼ 1 2 [11]. Our final step is therefore to solve the gap equation for the secondary pairing strength ∆ s as a function of β,…”

Section: The Action For the Quarks Ismentioning

confidence: 99%

“…We give a detailed treatment of secondary pairing in the Cγ 0 γ 5 channel, because it is the only one that, for a single color and single flavor, is predicted to be attractive under an NJL interaction based on single gluon exchange (Ref. [11], last 4 lines of Table 2). We work at zero temperature throughout.…”

Section: Introductionmentioning

confidence: 99%

Secondary pairing in gapless colour-superconducting quark matter

Alford¹,

Wang²

2005

J. Phys. G: Nucl. Part. Phys.

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We calculate secondary pairing in a model of a color superconductor with a quadratic gapless dispersion relation for the quasiquarks of the primary pairing. Our model mimics the physics of the sector of blue up and red strange quarks in gapless color-flavorlocked quark matter. The secondary pairing opens up a gap ∆ s in the quark spectrum, and we confirm Hong's prediction that in typical secondary channels ∆ s ∝ G 2 s for coupling strength G s . This shows that the large density of states of the quadratically gapless mode greatly enhances the secondary pairing over the standard BCS result ∆ ∝ exp(−const/G). In all of the secondary channels that we analyzed we find that the secondary gap, even with this enhancement, is from ten to hundreds of times smaller than the primary gap at reasonable values of the secondary coupling, indicating that secondary pairing does not generically resolve the magnetic instability of the gapless phase.

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“…Equal spin (isospin, flavor) pairing is another option, if the interaction between the same spin particles is attractive [22][23][24]. Since the separation of the Fermi surfaces does not affect the spin-1 pairing on each Fermi surface, an asymmetric superconductor evolves into a spin-1 superconducting state (rather than a non-superconducting state) as the asymmetry is increased.…”

Section: Alternativesmentioning

confidence: 99%

Superconductivity With Deformed Fermi Surfaces and Compact Stars

Sedrakian¹

2006

NATO Science Series II: Mathematics, Physics and Chemistry

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I discuss the deformed Fermi surface superconductivity (DFS) and some of its alternatives in the context of nucleonic superfluids and two flavor color superconductors that may exist in the densest regions of compact stellar objects. IntroductionThe astrophysical motivation to study the superconducting phases of dense matter arises from the importance of pair correlations in the observational manifestations of dense matter in compact stars. If the densest regions of compact stars contain deconfined quark matter it must be charge neutral and in β equilibrium with respect to the Urca processes d → u + e +ν and u + e → d + ν, where e, ν, andν refer to electron, electron neutrino, and antineutrino. The u and d quarks in deconfined matter fill two different Fermi spheres which are separated by a gap of the order of electron chemical potential. At high enough densities (where the typical chemical potentials become of the order of the rest mass of a s quark), strangeness nucleation changes the equilibrium composition of the matter via the reactions s → u + e +ν and u + e → s + ν. Although the strangeness content of matter affects its u-d flavor asymmetry, the separation of the Fermi energies remains a generic feature. The dense quark matter is expected to be a color superconductor (the early work is in Refs. [1]; recent developments are summarized in the reviews [2]).Accurate description of the matter in this regime requires, first, tools to treat the Lagrangian of QCD in the nonperturbative regime and, second, an understanding of the superconductivity under asymmetry in the population of fermions that pair. The first principle lattice QCD calculations are currently not feasible for the purpose of understanding the physics of compact stars; the effective models that are used rarely incorporate all aspects of the known phenomenology like de-confinement and chiral restoration. Despite of the limitations of current models, a lot can be learned about generic features of possible

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Single color and single flavor color superconductivity

Cited by 105 publications

References 54 publications

Rapid cooling of Cassiopeia A as a phase transition in dense QCD

Rapid cooling of Cassiopeia A as a phase transition in dense QCD

Secondary pairing in gapless colour-superconducting quark matter

Superconductivity With Deformed Fermi Surfaces and Compact Stars

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