R-mode oscillations of differentially and rapidly rotating Newtonian polytropic stars

摘要: For analysis of the r-mode oscillation hot young neutron stars, it is necessary to consider effect differential rotation, because viscosity not strong enough for differentially rotating stars be led uniformly configurations on a very short time scale after their birth. In this paper, we have developed numerical scheme solve oscillations polytropic inviscid stars. This extended version method which was applied compute Newtonian By using new method, succeeded in obtaining eigenvalues and eigenfunctions Our results show that as degree rotation increased, becomes more difficult slightly deformed from sphere compared solving considerably One reason seems corotation cylinder appears near stellar surface region if large enough. similar situation perturbational approach low-frequency slowly general relativity singular eigenvalue problem.