Collective Modes in the Superfluid Inner Crust of Neutron Stars

Abstract

The neutron-star inner crust is assumed to be superfluid at relevant temperatures. The contribution of neutron quasiparticles to thermodynamic and transport properties of the crust is therefore strongly suppressed by the pairing gap. Nevertheless, the neutron gas still has low-energy excitations, namely long-wavelength collective modes. We summarize different approaches to describe the collective modes in the crystalline phases of the inner crust and present an improved model for the description of the collective modes in the pasta phases within superfluid hydrodynamics.

20 pages, 9 figures

References in corpus (12)

• Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter
• Neutron conduction in the inner crust of a neutron star in the framework of the band theory of solids
• The pasta phase within density dependent hadronic models
• Low-energy collective excitations in the neutron star inner crust
• Superfluid Heat Conduction and the Cooling of Magnetized Neutron Stars
• Entrainment parameters in cold superfluid neutron star core
• The relativistic entrainment matrix of a superfluid nucleon-hyperon mixture at zero temperature
• Theory of cooling neutron stars versus observations
• Collective Modes in a Superfluid Neutron Gas within the Quasiparticle Random-Phase Approximation
• Temperature and finite-size effects in collective modes of superfluid Fermi gases
• Collective Excitations of Trapped Imbalanced Fermion Gases
• Response functions of cold neutron matter: density, spin and current fluctuations

Cited by in corpus (6)

• Superfluidity in nuclear systems and neutron stars
• Superfluid hydrodynamics in the inner crust of neutron stars
• Numerical models for stationary superfluid neutron stars in general relativity with realistic equations of state
• Long-wavelength phonons in the crystalline and pasta phases of neutron-star crusts
• Shape stability of pasta phases: Lasagna case
• Dynamical scheme for computing the mass parameter of a system in a medium