Axial quasinormal modes of neutron stars in R2 gravity

In the present paper, the axial quasinormal modes of neutron stars in f(R) gravity are examined using a large set of equations of state. The numerical calculations are made using two different approaches: performing time evolution of the perturbation equations and solving the time-independent representation of the equations as a boundary value problem. According to the results, the mode frequencies and the damping times decrease with the increase of the free parameter of the theory in comparison to the pure general relativistic case. While the frequencies deviate significantly from Einstein's theory for all realistic neutron star masses (say above 1 M-circle dot), the damping times reach non-negligible differences only for the more massive models. We have constructed as well universal (equation of state-independent) gravitational wave asteroseismology relations involving the frequencies and the damping times. It turns out that the equation-of-state independence is preserved using the same normalization as in pure general relativity. We discuss the differences of the phenomenological relations with respect to Einstein's theory of gravity for several values of the free parameter in f(R) gravity.