Collective Modes in the Superfluid Inner Crust of Neutron Stars
Michael Urban, Micaela Oertel
TL;DR
This paper reviews and improves models for collective excitations in the superfluid inner crust of neutron stars, focusing on the pasta phases and their impact on thermodynamic and transport properties.
Contribution
It introduces an enhanced superfluid hydrodynamics model for describing collective modes in the complex pasta phases of neutron star crusts.
Findings
Identification of low-energy collective modes in neutron star crusts
Improved modeling of pasta phase collective excitations
Insights into the role of these modes in neutron star physics
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.
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