English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

In this paper, the implications of the symmetry energy on the hadron andquark phase transitions in the compact star, including the properties of thepossible configurations of the quark-hadron hybrid stars, are investigated inthe frameworks of the energy-density functional (EDF) models and the flavorSU(2) Nambu--Jona-Lasinio (NJL) model with the help of the Schwinger'scovariant proper-time regularization (PTR) scheme. In this {theoretical setup},the equations of states (EoSs) of hadronic matter for various values ofsymmetry energies obtained from the EDF models are employed to describe thehadronic matter, and the {flavor} SU(2) NJL model with various repulsive-vectorinteraction strengths are used to describe the quark matter. We then observethe obtained EoS in the mass-radius properties of the hybrid starconfigurations for various vector interactions and nuclear symmetry energies bysolving the Tolman-Oppenheimer-Volkoff equation. We obtain that the criticaldensity at which the phase transition occurs varies over the density(3.6--6.7)$\rho_0$ depending on the symmetry energy and the strength of thevector coupling $G_v$. The maximum mass of the neutron star (NS) is susceptibleto $G_v$. When there is no repulsive force, the NS maximum mass is only about$1.5M_\odot$, but it becomes larger than $2.0M_\odot$ when the vector couplingconstant is about half of the {attractive} scalar coupling constant.Surprisingly, the presence of the quark matter does not affect the canonicalmass of NS ($1.4M_\odot$), so observing the canonical mass of NSs can provideunique constraints to the EoS of hadronic matter at high densities.

Effects of Symmetry Energy on the Equation of State for Hybrid Neutron Stars