In this Review we study the nuclear pastas as they are expected to be formed in neutron star cores. We start with a study of the pastas formed in nuclear matter (composed of protons and neutrons), we follow with the role of the electron...
moreIn this Review we study the nuclear pastas as they are expected to be formed in neutron star cores. We start with a study of the pastas formed in nuclear matter (composed of protons and neutrons), we follow with the role of the electron gas on the formation of pastas, and we then investigate the pastas in neutron star matter (nuclear matter embedded in an electron gas). T 15 MeV), at saturation and sub-saturation densities, and with proton content ranging from 30% to 50% was found to have liquid, gaseous and liquid-gas mixed phases. The isospin-dependent phase diagram was obtained along with the critical points, and the symmetry energy was calculated and compared to experimental data and other theories. At low temperatures (T 1 MeV) NM produces crystal-like structures around saturation densities, and pasta-like structures at sub-saturation densities. Properties of the pasta structures were studied with cluster-recognition algorithms, caloric curve, the radial distribution function, the Lindemann coefficient, Kolmogorov statistics, Minkowski functionals; the symmetry energy of the pasta showed a connection with its morphology. Neutron star matter (NSM) is nuclear matter embedded in an electron gas. The electron gas is included in the calculation by the inclusion of an screened Coulomb potential. To connect the NM pastas with those in neutron star matter (NSM), the role the strength and screening length of the Coulomb interaction have on the formation of the pastas in NM was investigated. Past was found to exist even without the presence of the electron gas, but the effect of the Coulomb interaction is to form more defined pasta structures, among other effects. Likewise, it was determined that there is a minimal screening length for the developed structures to be independent of the cell size. Neutron star matter was found to have similar phases as NM, phase transitions, symmetry energy, structure function and thermal conductivity. Like in NM, pasta forms at around T ≈ 1.5 MeV, and liquid-to-solid phase changes were detected at T ≈ 0.5 MeV. The structure function and the symmetry energy were also found to depend on the pasta structures. A. The pasta B. The pasta in nuclear matter and in neutron star matter II. Nuclear matter A. Nuclear matter at intermediate temperatures B. Nuclear matter at low temperatures C. Summary of nuclear matter properties III. Electron gas: connecting nuclear matter with neutron star matter A. The strength of V C B. The screening length C. Summarizing the electron gas IV. Neutron star matter A. Symmetric neutron star matter B. Non-symmetric neutron star matter C. The symmetry energy D. Neutrino transport properties E. Properties of non-traditional pasta F. The nucleon thermal conductivity G. Summary of NSM properties V. Conclusion A. Nuclear matter B. The electron gas C. The pasta in neutron star matter VI. Appendices A. Classical Molecular Dynamics B. The Maxwell construction C. Nuclear symmetry energy from CMD at intermediate temperatures D. Nuclear symmetry energy from CMD at low temperatures E. Symmetry energy for neutron star matter F. Thermal conductivity G. Analytical tools 1. The Radial Distribution Function 2. Lindemann coefficient 3. Kolmogorov statistic 4. Minkowski functionals 5. The Minkowski voxels 6. Cluster recognition In this review we will use the classical molecular dynamics model (CMD) to study the pasta in nuclear matter and in neutron star matter; systems which will be defined in the next Section. To avoid technical distractions, the description of the CMD model is relegated to Appendix A. The neutron star crust is composed of protons, neutrons and an embedding gas of electrons. To study such system we systematically divide the review in three parts. First, a study of nuclear matter (NM), e.g. systems composed solely of protons and neutrons; second, an investigation of the role electrons have on the properties of NM; and third, a study of neutron star matter (NSM), i.e. systems of protons and neutrons embedded in an electron gas. Nuclear matter exhibits fascinating complex phenomena at subsaturation densities and warm and cold temperatures. At densities below the saturation density, ρ 0 = 0.16 fm -3 , and temperatures, say, between 1 MeV and 5 MeV, nuclear systems exist in liquid and gaseous phases, as well as in a mixture between the two. At lower temperatures, crystals and structures resembling the so-called nuclear pastas appear with different morphologies depending on the temperature, density and isospin content and, furthermore, nucleons inside such structures can undergo phase transitions. This review studies nuclear matter first. At intermediate temperatures we review the bulk properties, phases and phase transitions of NM, all with varying percentages of isospin content to allow the study of the symmetry energy. At lower energies, the formation of the pasta is investigated along with its properties, phases, transitions, and symmetry energy. This is followed by a review of the role the electron gas has on the pasta of nuclear matter. As the electron gas is introduced in the CMD calculation by means of a screened Coulomb potential, the study focuses on the effects the strength and range of the interaction have on the morphology of the pastas. Finally, the properties of the pastas in neutron star matter, i.e. systems with protons, neutrons and electrons, are reviewed with special attention to their shapes, phases, phase transitions, and symmetry energy. In understanding the pastas both in NM and in NSM we also study how the energy varies with respect to the isospin content, i.e. the symmetry energy. It is in this type of studies that one can appreciate the value of CMD, as to perform such a study at intermediate and low temperatures and sub-saturation densities, a model capable of exhibiting clustering phenomena and phase changes is needed. Similarly, as mentioned before, the cooling of neutron stars is related to pasta structure of the crust as the neutrino opacity is enhanced by coherent scattering. Here, we also study the very-long range order of the pasta phases, focusing on its influence on the opacity of the crust to low-momentum neutrinos. In this review the properties of nuclear matter will be studied in Section II, the role of the electron gas on the NM will be investigated in Section III and, finally, the neutron star matter will be studied in Section IV. Analytical tools used, such as the classical molecular dynamics method used, algorithms for the recognition of clusters, the radial correlation functions, Lindemann coefficient, Kolmogorov statistics, Minkowski functionals, and the procedure used to calculate the symmetry energy are presented in the various appendices.