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

The effect of isospin-dependent nuclear forces on the inner crust of neutronstars is modeled within the framework of Quantum Molecular Dynamics (QMD). Tosuccessfully control the density dependence of the symmetry energy ofneutron-star matter below nuclear saturation density, a coupling potentialbetween the $\omega$ and $\rho$ meson fields is introduced. This approach isinspired by the baryon density and isospin density-dependent repulsive Skyrmeforce of asymmetric nuclear matter. In isospin-asymmetric nuclear matter, thesystem shows nucleation, as nucleons are arranged into shapes resemblingnuclear pasta. The dependence of clusterization in the system on the isospinproperties is also explored by calculating two-point correlation functions. Weshow that, as compared to previous results that did not involve the$\omega$-$\rho$ potential, the energy symmetry slope $L$ is successfullycontrolled by varying the $\omega$-$\rho$ coupling strength. Nevertheless, theeffect of changing the slope of the nuclear symmetry energy $L$ on thecrust-core transition density does not seem significant. To the knowledge ofthe authors, This is the first implementation of a $\omega$-$\rho$ coupling ina QMD model for the inner crust of neutron stars.

Low Density Neutron Star Matter with Quantum Molecular Dynamics: The Role of Vector Interactions