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

We delineate the quark-hadron continuity by constructing QCD equations ofstate for neutron star dynamics, covering the wide range of charge chemicalpotential ($\mu_Q$) and temperatures ($T$). Based on the nuclear-2SC continuityscenario, we match equations of state for nuclear and two-flavorcolor-superconducting (2SC) quark matter, where the matching baryon density is$n_B\simeq 1.5n_0$ ($n_0\simeq 0.16\, {\rm fm^{-3}}$: nuclear saturationdensity). The effective vector and diquark couplings in a quark matter modelevolve as functions of $n_B, \mu_Q, T$, whose low density values areconstrained by the nuclear matter properties and neutron star radii, with thehigh density behavior by the two-solar mass ($2M_\odot$) constraint. Withcouplings dependent on $n_B$, we examined how smooth the nuclear-2SC continuitycan be, and found problems in matching nuclear and 2SC entropies at lowtemperatures. To proceed with the continuity scenario, we enforce smoothmatching by making the couplings ($n_B, \mu_Q, T$)-dependent. In effect, thisadds phenomenological contributions which we call "X". After thephenomenological matching, we take the rest as our predictions. The 2SC andcolor-flavor-locked (CFL) phases computed with these evolving couplings arecalled 2SCX and CFLX. The CFLX appears around $n_B\simeq 2$-$4n_0$ and, incontrast to the conventional CFL, has non-negligible dependence on $(\mu_Q,T)$.To examine the astrophysical consequences of our modeling, we add chargedleptons and neutrinos, and study the composition of matter for lepton fractionsrelevant for protoneutron stars and neutron star mergers. The abundance ofneutrinos and thermal effects reduce the strangeness fraction and stiffenequations of state. For a neutrino trapped neutron star at $T\simeq 30 $ MeVwith a lepton fraction $Y_L\simeq 0.05$, the mass is larger than its coldstatic counterpart by $\sim 0.1M_\odot$.

Phenomenological QCD equations of state for neutron star dynamics: Nuclear-2SC continuity and evolving effective couplings