Neutron Stars and Massive Quark Matter

Abstract

Using the Color-Dielectric model to describe quark confinement, including strange quarks and accounting for beta--equilibrium, we get masses for a static neutron star in the range $1.3\le M/M_{\odot }\le 1.54$ for a radius $R\approx 9$ km. Rapid cooling through the direct URCA mechanism is obtained. The implications for the composition of neutron stars is discussed.

8 pages, Revtex style, 4 uuencoded figures appended

References in corpus (8)

• Phase Transitions in Warm, Asymmetric Nuclear Matter
• Strangeness in Hadronic Stellar Matter
• Asymmetric nuclear matter and neutron star properties
• High density QCD with static quarks
• Observational constraints on the neutron star mass distribution
• Geminga: A Cooling Superfluid Neutron Star
• Quark Matter in the Chiral Color Dielectric Model
• Muons and emissivities of neutrinos in neutron star cores

Cited by in corpus (20)

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• Exploring physical features of anisotropic strange stars beyond standard maximum mass limit in $f\left(R,\mathcal{T}\right)$ gravity
• Hybrid stars with the color dielectric and the MIT bag models
• A dynamical, confining model and hot quark stars
• Quark magnetar in three-flavor Nambu--Jona-Lasinio model with vector interaction and magnetized gluon potential
• A confinement model calculation of h_1(x)
• Finite Temperature Quark Matter and Supernova Explosion
• Metastable strange matter and compact quark stars
• Chiral model approach to quark matter nucleation in neutron stars
• Role of Curvature-Matter Coupling on Anisotropic Strange Stars
• Recoil effects on nucleon electromagnetic form factors
• Timing evolution of accreting strange stars
• Conditions for the existence of stable strange quark matter
• Strong magnetic field in a protoneutron star
• The Equation of State of Dense Matter : from Nuclear Collisions to Neutron Stars
• Hybrid stars : Spin polarised nuclear matter and density dependent quark masses
• Neutron Stars, Supernova Explosions and the Transition to Quark Matter