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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Properties of $\Lambda,~\Xi^0$ hypernuclei and neutron stars are investigatedin quark mean field model with pion and gluon corrections. Firstly, $u, ~d$,and $s$ quarks are confined by relativistic harmonic oscillator potentials togenerate the baryons, like nucleon, $\Lambda, ~\Sigma$, and $\Xi$ hyperons. Theeffects of pion-quark coupling and one-gluon exchange are consideredperturbatively. Then, the baryons interact with each other through exchanging$\sigma, ~\omega,$ and $\rho$ mesons between quarks in hypernuclei and nuclearmatter. The strengths of confinement potentials for $u, ~d,$ and $s$ quarks aredetermined by the masses and radii of free baryons. The coupling constantsbetween the quarks and mesons are fixed by the ground-state properties ofseveral nuclei and single-hyperon potentials at nuclear saturation density,which arises three parameter sets for the coupling constants between mesons andquarks, named QMF-NK1S, QMF-NK2S, and QMF-NK3S. Compared to the results ofprevious quark mean field model without pion and gluon corrections, it is foundthat properties of $\Lambda$ hypernuclei, i.e. the single $\Lambda$ energies,are more consistent with the experimental observables. Properties of $\Xi^0$hypernuclei are also calculated and compared with the results in previous quarkmean field model. With these three parameter sets, the neutron stars containinghyperons are investigated through solving the Tolman-Oppenheimer-Volkoffequation. Maximum masses of neutron stars approach $2.1M_\odot$ with hyperonsand corresponding radii are around $13$ km.

Quark mean field model with pion and gluon corrections for $\Lambda,~\Xi^0$ hypernuclei and neutron stars