Spin polarization and color superconductivity in quark matter

Nakano, Eiji; Maruyama, Tomoyuki; Tatsumi, Toshitaka

doi:10.1103/physrevd.68.105001

Cited by 70 publications

(101 citation statements)

References 41 publications

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“…Note also that one should distinguish between the spontaneous deformation of Fermi-surfaces and explicit breaking of rotational symmetry by external fields. In the latter case the initial Lagrangian contains term(s) that explicitely break the symmetry and the resulting anisotropy of the self-energies can be interpreted as a deformation of the Fermi surfaces [19]. These type of deformations are interaction induced and are unrelated to the spontaneous deformations that appear even if the interaction is O(3) symmetric.…”

Section: Dfs Phasementioning

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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Section: Dfs Phasementioning

confidence: 99%

Superconductivity With Deformed Fermi Surfaces and Compact Stars

Sedrakian¹

2006

NATO Science Series II: Mathematics, Physics and Chemistry

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“…We have considered the possibility of ferromagnetism in quark matter interacting with the one-gluon-exchange (OGE) interaction [5] or with an effective interaction [6], and suggested that quark matter has a potentiality to be spontaneously polarized. To understand the magnetic properties of quark matter more realistically , especially near the critical point, some non-perturbative consideration about the instability of the Fermi surface is indispensable.…”

Section: Relativistic Ferromagnetismmentioning

confidence: 99%

Microscopic origin of the magnetic field in compact stars

Tatsumi¹

2006

AIP Conference Proceedings

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“…The choice of M M determines detection efficiencies and waveform parameter resolutions. Some template construction methods for a given M M have already been proposed as [19], [20,21]. In a realistic search, however, non-stationary noises in detector outputs would reduce SNRs, so it is not clear whether the criterion ≥ M M is still fulfilled.…”

Section: Introductionmentioning

confidence: 99%

“…Arnaud et al discussed a general template construction method for matched filtering searches and its application to the ringdown case [19]. Recently Nakano et al proposed an efficient tiling method for ringdown filters [20,21].…”

Section: Introductionmentioning

confidence: 99%

“…The ringdown signals with randomly selected waveform parameters are injected into TAMA300 data by software, and filtered with the template bank. We employ the template spacing method recently proposed by Nakano et al [20,21], which provides an efficient tiling scheme to cover the parameter space with a fewer templates keeping the criterion ≥ M M . For gravitational wave sources, we consider black holes distributed in the Galaxy, since magnitudes of ringdown waves from distances of Galactic scales (∼ 10 kpc) are expected enough large to be detected with contemporary interferometors as TAMA300 ( see FIG.…”

Section: Introductionmentioning

confidence: 99%

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On detection of black hole quasinormal ringdowns: Detection efficiency and waveform parameter determination in matched filtering

et al. 2005

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Gravitational radiation from a slightly distorted black hole with ringdown waveform is well understood in general relativity. It provides a probe for direct observation of black holes and determination of their physical parameters, masses and angular momenta (Kerr parameters). For ringdown searches using data of gravitational wave detectors, matched filtering technique is useful. In this paper, we describe studies on problems in matched filtering analysis in realistic gravitational wave searches using observational data. Above all, we focus on template constructions, matches or signal-to-noise ratios (SNRs), detection probabilities for Galactic events, and accuracies in evaluation of waveform parameters or black hole hairs. In template design for matched filtering, search parameter ranges and template separations are determined by requirements from acceptable maximum loss of SNRs, detection efficiencies, and computational costs. In realistic searches using observational data, however, effects of non-stationary noises cause decreases of SNRs, and increases of errors in waveform parameter determinations. These problems will potentially arise in any matched filtering searches for any kind of waveforms. To investigate them, we have performed matched filtering analysis for artificial ringdown signals which are generated with Monte-Carlo technique and injected into the TAMA300 observational data. We employed an efficient method to construct a bank of ringdown filters recently proposed by Nakano et al., and use a template bank generated from a criterion such that losses of SNRs of any signals do not exceed 2%. We found that this criterion is fulfilled in ringdown searches using TAMA300 data, by examining distribution of SNRs of simulated signals. It is also shown that with TAMA300 sensitivity, the detection probability for Galactic ringdown events is about 50% for black holes of masses greater than 20M⊙ with SNR > 10. The accuracies in waveform parameter estimations are found to be consistent with the template spacings, and resolutions for black hole masses and the Kerr parameters are evaluated as a few % and ∼ 40%, respectively. They can be improved up to < 0.9% and < 24% for events of SNR ≥ 10 by using fine-meshed template bank in the hierarchical search strategy.

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Spin polarization and color superconductivity in quark matter

Cited by 70 publications

References 41 publications

Superconductivity With Deformed Fermi Surfaces and Compact Stars

Superconductivity With Deformed Fermi Surfaces and Compact Stars

Microscopic origin of the magnetic field in compact stars

On detection of black hole quasinormal ringdowns: Detection efficiency and waveform parameter determination in matched filtering

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