Impact of the equation of state on f  and p  mode oscillations of neutron stars
Abstract
We investigate the impact of the neutronstar matter equation of state on the f  and p_{1}mode oscillations of neutron stars obtained within the Cowling approximation and linearized general relativity. The f  and p_{1}mode oscillation frequencies, and their damping times are calculated using representative sets of Skyrme HartreeFock and relativistic meanfield models, all of which reproduce nuclear systematics and support 2 M_{⊙} neutron stars. Our study shows strong correlations between the frequencies of f  and p_{1}modes and their damping times with the pressure of β equilibrated matter at densities equal to or slightly higher than the nuclear saturation density ρ_{0}. Such correlations are found to be almost independent of the composition of the stars. The frequency of the p_{1}mode of 1.4 M_{⊙} star is strongly correlated with the slope of the symmetry energy L_{0} and β equilibrated pressure at density ρ_{0}. Compared to GR calculations, the error in the Cowling approximation for the f mode is about 30% for neutron stars of low mass, whereas it decreases with increasing mass. The accuracy of the p_{1}mode is better than 15% for neutron stars of maximum mass, and improves for lower masses and higher number of radial nodes.
 Publication:

Physical Review D
 Pub Date:
 September 2022
 DOI:
 10.1103/PhysRevD.106.063005
 arXiv:
 arXiv:2205.02081
 Bibcode:
 2022PhRvD.106f3005K
 Keywords:

 Nuclear Theory;
 General Relativity and Quantum Cosmology
 EPrint:
 Comments are welcome