Theoretical Physics Colloquium
Aspects of neutron superfluidity in the neutron star inner crust
by Dr. Rishi Sharma (TRIUMF, Canada)
Tuesday, July 24, 2012
from
to
(Asia/Kolkata)
at Colaba Campus ( AG69 )
at Colaba Campus ( AG69 )
Description |
The inner crust of a neutron star is expected to feature a lattice of neutron rich nuclei in a sea of unbound neutrons. The unbound neutrons form pairs and are superfluid. I will describe the low energy effective theory describing the dynamics of this phase of dense matter, applicable up to temperatures of about a billion Kelvins. Using the theory, we calculate the heat conductivity due to superfluid phonons, a collective mode of the superfluid neutron gas, and consider the implications for crustal heat transport in neutron stars. Due to the large scattering length between neutrons, the strongly coupled (unitary) Fermi gas is an interesting model for the neutron superfluid. I will describe a calculation of the response of the unitary Fermi gas to density fluctuations, which can be related to the coefficients of the low energy theory in the absence of the lattice. |
Material: |