Stability of the mixed phase in hybrid stars

Abstract

The transition from hadronic matter to quark matter in the core of neutron stars is likely to be associated with the appearance of a mixed phase, leading to a smooth variation of the star density profile. We discuss the results of a systematic study of the properties of the mixed pase upon Coulomb and surface effects. A state of the art nonrelativistic equation of state of nuclear matter has been used for the low density phase, while quark matter has been described within the MIT bag model, including the effect of perturbative one-gluon exchange interactions. The implications for neutron star structure are discussed.

Submitted to Astronomy & Astrophysics

References in corpus (4)

• Quantum Monte Carlo Calculations of Light Nuclei
• Gravitationally redshifted absorption lines in the X-ray burst spectra of a neutron star
• The mass of the neutron star in Vela X-1 and tidally induced non-radial oscillations in GP Vel
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Cited by in corpus (8)

• The Nuclear Symmetry Energy
• Quark matter imprint on Gravitational Waves from oscillating stars
• A Detailed Analysis of the Special Points on $M-R$ Solutions of Hybrid (Twin) Stars
• Effects of hadron-quark phase transition on properties of Neutron Stars
• Properties of Hybrid Stars with Density Dependent Bag Model
• Deconfinement of non-strange hadronic matter with nucleons and $\Delta$ baryons to quark matter in neutron stars
• Analyzing the dense matter equation of states in the light of the compact object HESS J1731-347
• Neutron star matter equation of state and gravitational wave emission