2015/05/26 by Armen Sedrakian, J. W. Clark, Sedrakian, Armen +2
Earth and Planetary Sciences · Physics and Astronomy · #Atomic and Subatomic Physics Research #FOS: Physical sciences #High-pressure geophysics and materials #Nuclear Theory (nucl-th) #Quantum, superfluid, helium dynamics #nucl-th
paper · pdf · doi:10.48550/arxiv.1505.06935
article style 8 pages, including 3 figures. Proceedings of "Compact Stars in the QCD Phase Diagram IV" (CSQCD IV), September 26-30, 2014, Prerow, Germany; v2: minor adjustments
openalex publication_date 2015/05/26 · arxiv created 2015/05/30 · arxiv updated 2016/01/26 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In this contribution we first review a method for obtaining the collective modes of pair-correlated neutron matter as found in a neutron star inner crust. We discuss two classes of modes corresponding to density and spin perturbations with energy spectra ω= ω0 + αq2, where ω0 = 2Δ is the threshold frequency and Δ is the gap in the neutron fluid spectrum. For characteristic values of Landau parameters in neutron star crusts the exitonic density modes have α< 0, therefore they live below the pair-breaking continuum ω0 and are undamped. For spin diffusive modes α> 0 and they exist above ω0 which implies that these modes are damped. As an application of these findings we compute the thermal conductivity due to spin diffusive modes and show that it scales as T1/2 exp(-2ω0/T) in the case where their two-by-two scattering cross-section is weakly dependent on temperature.