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

One of the most promising possibilities may be the appearance of quark matterin astrophysical phenomena in the light of recent progress in observations. Themechanism of deconfinement is not well understood, but the thermodynamicalaspects of the hadron-quark (HQ) phase transition have been extensively studiedin recent years. Then the mixed phase of hadron and quark matter becomesimportant; the proper treatment is needed to describe the HQ phase transitionand derive the equation of state (EOS) for the HQ matter, based on the Gibbsconditions for phase equilibrium. We here adopt a EOS based on thebaryon-baryon interactions including hyperons for the hadron phase, while weuse rather simple EOS within the MIT bag model in the quark phase. For quarkmatter we further try to improve the previous EOS by considering othereffective models of QCD. One of the interesting consequences may be theappearance of the inhomogeneous structures called "pasta", which are broughtabout by the surface and the Coulomb interaction effects. We present here acomprehensive review of our recent works about the HQ phase transition invarious astrophysical situations: cold catalyzed matter, hot matter andneutrino-trapped matter. We show how the pasta structure becomes unstable bythe charge screening of the Coulomb interaction, thermal effect or the neutrinotrapping effect. Such inhomogeneous structure may affect astrophysicalphenomena through its elasticity or thermal properties. Here we also discusssome implications on supernova explosion, gravitational wave and cooling ofcompact stars.

Thermodynamical description of hadron-quark phase transition and its implications on compact-star phenomena