Description
Neutron stars are studied with hydrodynamical equations that govern their macroscopic behavior. The relaxation times to any external perturbations to the star are controlled by the transport coefficients that enter into the hydrodynamical equations, such us the bulk and shear viscosities or the thermal conductivity. The value of these coefficients depend on the microscopic physics of the star, and thus their knowledge can provide us with very valuable information of the neutron star’s interiors.
