Phoebe Hänsel

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We study the consequences of recent progress in the experimental determination of masses of neutron rich nuclei for our knowledge of the ground state of cold dense matter. The most recent experimental data determine the ground state of cold dense matter up to ρ ≃ 10 11 g cm −3. The composition and the equation of state of the ground state of matter, in this(More)
New calculations of the thermal and electrical electron conductivities are performed for a broad range of physical parameters typical for envelopes of neutron stars and cores of white dwarfs. We consider stellar matter composed of astrophysically important chemical elements from H to Fe in the density range from 10 2 { 10 4 g cm ?3 up to 10 7 {10 10 g cm ?3(More)
We simulate the cooling of the neutron star in the X-ray transient KS 1731–260 after the source returned to quiescence in 2001 from a long (& 12.5 yr) outburst state. We show that the cooling can be explained assuming that the crust underwent deep heating during the outburst stage. In our best theoretical scenario the neutron star has no enhanced neutrino(More)
Cooling simulations of neutron stars (NSs) are performed assuming that stellar cores consist of neutrons, protons and electrons and using realistic density profiles of superfluid critical temperatures Tcn(ρ) and Tcp(ρ) of neutrons and protons. Taking a suitable profile of Tcp(ρ) with maximum ∼5 × 10 9 K one can obtain smooth transition from slow to rapid(More)
The bulk viscosity of neutron star cores containing hyperons is studied taking into account nonequilibrium weak process n + n ⇀↽ p + Σ−. The rapid growth of the bulk viscosity within the neutron star core associated with switching on new reactions (modified Urca process, direct Urca process, hyperon reactions) is analyzed. The suppression of the bulk(More)
Analytical representations are derived for two equations of state (EOSs) of neutron-star matter: FPS and SLy. Each of these EOSs is unified, that is, it describes the crust and the core of a neutron star using the same physical model. Two versions of the EOS parametrization are considered. In the first one, pressure and mass density are given as functions(More)