Superfluid Heat Conduction and the Cooling of Magnetized Neutron Stars

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dc.creatorAguilera, Deborah N.
dc.creatorCirigliano, Vincenzo
dc.creatorPons, José A.
dc.creatorReddy, Sanjay
dc.creatorSharma, Rishi
dc.date2008-07-29
dc.date.accessioned2026-07-07T13:01:00Z
dc.date.available2026-07-07T13:01:00Z
dc.descriptionWe report on a new mechanism for heat conduction in the neutron star crust. We find that collective modes of superfluid neutron matter, called superfluid phonons (sPhs), can influence heat conduction in magnetized neutron stars. They can dominate the heat conduction transverse to magnetic field when the magnetic field $B \gsim 10^{13}$ G. At density $ρ\simeq 10^{12}-10^{14} $ g/cm$^3$ the conductivity due to sPhs is significantly larger than that due to lattice phonons and is comparable to electron conductivity when temperature $\simeq 10^8$ K. This new mode of heat conduction can limit the surface anisotropy in highly magnetized neutron stars. Cooling curves of magnetized neutron stars with and without superfluid heat conduction could show observationally discernible differences.
dc.description4 pages, 3 figures
dc.identifierhttps://arxiv.org/abs/0807.4754
dc.identifierhttp://arxiv.org/abs/0807.4754
dc.identifierPhys.Rev.Lett.102:091101,2009
dc.identifierdoi:10.1103/PhysRevLett.102.091101
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/226023
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleSuperfluid Heat Conduction and the Cooling of Magnetized Neutron Stars
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