Dynamical relativistic RPA calculations predict lower crust-core transition densities and pressures than thermodynamic ones across covariant energy density functionals, resulting in thinner crusts and reduced crustal moment of inertia fractions.
Dynamical Simulation of Nuclear "Pasta": Soft Condensed Matter in Dense Stars
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abstract
More than twenty years ago, it was predicted that nuclei can adopt interesting shapes, such as rods or slabs, etc., in the cores of supernovae and the crusts of neutron stars. These non-spherical nuclei are referred to as nuclear "pasta". In recent years, we have been studying the dynamics of the pasta phases using a method called quantum molecular dynamics (QMD) and have opened up a new aspect of study for this system. Our findings include: dynamical formation of the pasta phases by cooling down the hot uniform nuclear matter; phase diagrams in the density versus temperature plane; structural transitions between the pasta phases induced by compression and elucidation of the mechanism by which they proceed. In the present article, we given an overview of the basic physics and astrophysics of the pasta phases and review our works for readers in other fields.
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Thermodynamic versus Dynamical Description of the Neutron-Star Crust-Core Instability: Implications for Crustal Observables
Dynamical relativistic RPA calculations predict lower crust-core transition densities and pressures than thermodynamic ones across covariant energy density functionals, resulting in thinner crusts and reduced crustal moment of inertia fractions.