Finite size effects in hadron-quark phase transition by the Dyson-Schwinger method

Abstract

We study the hadron-quark phase transition, taking into account the finite-size effects for neutron star matter. For the hadron phase, we adopt a realistic equation of state within the framework of the Brueckner-Hartree-Fock theory. For the quark phase, we apply the Dyson-Schwinger method. The properties of the mixed phase are clarified by considering the finite-size effects. We find that, if the surface tension is strong enough, the equation of state becomes to be close the one with the Maxwell condition, though we properly adopt the Gibbs conditions. This result is qualitatively the same with the one by the use of the simple bag model. We also find that the mass-radius relation by the EoS is consistent with the observations of massive neutron stars.

4 pages, 2 figures, the proceeding for "Nuclear Physics in Astrophysics VI"

References in corpus (4)

• Shapiro delay measurement of a two solar mass neutron star
• Nuclear Force from Lattice QCD
• Hadron-quark mixed phase in hyperon stars
• Hybrid stars with the Dyson-Schwinger quark model

Cited by in corpus (8)

• Constraining strangeness in dense matter with GW170817
• Hybrid stars in light of the HESS J1731-347 remnant and the PREX-II experiment
• Phase Transitions in Neutron Stars
• Critical temperature of deconfinement in a constrained space using a bag model at vanishing baryon density
• Hadron-quark phase transition in neutron star by combining the relativistic Brueckner-Hartree-Fock theory and Dyson-Schwinger equation approach
• The stifness of the supranuclear equation of state (once again)
• On the Cooling of Compact Stars in Light of the HESS J1731-347 Remnant
• Cooling of Compact Stars with Color Superconducting Quark Matter