2014/11/27 by Laura Tolos, Cristina Manuel, Tolos, Laura +5
Physics and Astronomy · #FOS: Physical sciences #High Energy Physics - Phenomenology (hep-ph) #Nuclear Theory (nucl-th) #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR #hep-ph #nucl-th
paper · pdf · doi:10.48550/arxiv.1411.7622
9 pages, 5 figures, contribution to the proceedings of XI Quark Confinement and the Hadron Spectrum, September 8-12, 2014, Saint-Petersburg State University, Russia
arxiv created 2014/11/27 · arxiv updated 2014/12/01
We study the shear and bulk viscosity coefficients as well as the thermal conductivity as arising from the collisions among phonons in superfluid neutron stars. We use effective field theory techniques to extract the allowed phonon collisional processes, written as a function of the equation of state and the gap of the system. The shear viscosity due to phonon scattering is compared to calculations of that coming from electron collisions. We also comment on the possible consequences for r-mode damping in superfluid neutron stars. Moreover, we find that phonon collisions give the leading contribution to the bulk viscosities in the core of the neutron stars. We finally obtain a temperature-independent thermal conductivity from phonon collisions and compare it with the electron-muon thermal conductivity in superfluid neutron stars.