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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.
Highlights
The neutron stars (NS) are in general very complex objects that connect many different fields of research, from nuclear and particle physics and astrophysics to general relativity
These are interpreted in terms of energy density functional (EDF) theory and are most widely used methods in the construction of astrophysical equation of state (EOS)
It can account for the European Muon Collaboration (EMC) effect [24] as well as predict new observables [25, 26] through which it can be tested
Summary
The neutron stars (NS) are in general very complex objects that connect many different fields of research, from nuclear and particle physics and astrophysics to general relativity. With the radii less than 14 km and masses as high as two solar mass, these objects are among the densest in the Universe Starting from their outer layer, the crust, density of stellar matter increases very rapidly as we travel inwards to the deeper layers of a NS due to the very strong gravitational force which is around 1011 times stronger than what we experience on Earth. The nuclear lattice is immersed in the already present free electron gas and neutron gas, who’s presence marks the transition to the inner crust of a NS at density ρ ∼ 10−5 fm−3. The model is used to calculate the outer crust properties while remarks are made on the composition of neutron star inner crust and core.
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