Observations of massive (M ≈ 2.0 M_⊙) neutron stars (NSs), PSRs J1614−2230 and J0348+0432, rule out most of the models of nucleon–hyperon matter employed in NS simulations. Here, we construct three possible models of nucleon–hyperon matter consistent with the existence of 2 M_⊙ pulsars as well as with semi-empirical nuclear matter parameters at saturation, and semi-empirical hypernuclear data. Our aim is to calculate for these models all the parameters necessary for modelling dynamics of hyperon stars (such as equation of state, adiabatic indices, thermodynamic derivatives, relativistic entrainment matrix, etc.), making them available for a potential user. To this aim a general non-linear hadronic Lagrangian involving σωρϕσ* meson fields, as well as quartic terms in vector-meson fields, is considered. A universal scheme for calculation of the ℓ = 0, 1 Landau Fermi-liquid parameters and relativistic entrainment matrix is formulated in the mean-field approximation. Use of this scheme allow us to obtain numerical tables with the equation of state, Landau quasi-particle effective masses, adiabatic indices, the ℓ = 0, 1 Landau Fermi-liquid parameters, and the relativistic entrainment matrix for the selected models of nucleon–hyperon matter. These data are available online and suitable for numerical implementation in computer codes modelling various dynamical processes in NSs, in particular, oscillations of superfluid NSs and their cooling.

We study the cooling of superfluid neutron stars whose cores consist of nucleon matter with the Akmal—Pandharipande—Ravenhall (APR) equation of state

We examine radial oscillations of superfluid neutron stars at finite internal temperatures. For this purpose, we generalize the description of relati

We study the equation of state (EOS) of an accreting neutron star crust. Usually, such an EOS is obtained by assuming (implicitly) that the free (unbound) neutrons and nuclei in the inner crust move together. We argue that this assumption violates the condition ${\mu }_n^{\infty }=\text{const}$, required for hydrostatic (and diffusion) equilibrium of unbound neutrons (${\mu }_n^{\infty }$ is the redshifted neutron chemical potential). We construct a new EOS respecting this condition, working in the compressible liquid-drop approximation. We demonstrate that it is close to the catalyzed EOS in most of the inner crust, being very different from EOSs of accreted crust discussed in the literature. In particular, the pressure at the outer-inner crust interface does not coincide with the neutron drip pressure, usually calculated in the literature, and is determined by hydrostatic (and diffusion) equilibrium conditions within the star. We also find an instability at the bottom of the fully accreted crust that transforms nuclei into homogeneous nuclear matter. It guarantees that the structure of the fully accreted crust remains self-similar during accretion.

One of the effective mechanisms of neutrino energy losses in red giants, pre‐supernovae and in the cores of white dwarfs is the emission of neutrino–

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