Neutron stars from crust to core within the Quark-meson coupling model
arXiv:1912.03815 · doi:10.1051/epjconf/202023203001
Abstract
Recent years continue to be an exciting time for the neutron star physics, providing many new observations and insights to these natural laboratories of cold dense matter. To describe them, there are many models on the market but still none that would reproduce all observed and experimental data. The quark-meson coupling model stands out with its natural inclusion of hyperons as dense matter building blocks, and fewer parameters necessary to obtain the nuclear matter equation of state. The latest advances of the QMC model and its application to the neutron star physics will be presented, within which we build the neutron star's outer crust from finite nuclei up to the neutron drip line. The appearance of different elements and their position in the crust of a neutron star is explored and compared to the predictions of various models, giving the same quality of the results for the QMC model as for the models when the nucleon structure is not taken into account.
arXiv comment4 pages, 1 figure, conference proceedings HIAS2019
References in corpus (11)
- Nuclear Ground-State Masses and Deformations
- A Massive Pulsar in a Compact Relativistic Binary
- Nuclear ground-state masses and deformations: FRDM(2012)
- Equations of state for supernovae and compact stars
- Global performance of covariant energy density functionals: ground state observables of even-even nuclei and the estimate of theoretical uncertainties
- Cold uniform matter and neutron stars in the quark-mesons-coupling model
- Physical Origin of Density Dependent Force of the Skyrme Type within the Quark Meson Coupling Model
- Quark-Meson-Coupling (QMC) model for finite nuclei, nuclear matter and beyond
- Finite Nuclei in the Quark-Meson Coupling (QMC) Model
- Isovector Effects in Neutron Stars, Radii and the GW170817 Constraint
- Parameter Optimisation for the Latest Quark-Meson Coupling Energy Density Functional