Speaker
Description
Highly magnetized neutron stars with magnetic fields of $10^{15-16}$ G are promising candidates to be the observed soft gamma repeaters and X-ray pulsars. On the other hand, oscillations of perturbed neutron stars are closely related to the composition, structure, and equation of state of the star. Thus far, the numerical study of oscillations of magnetized neutron stars has not yet realized the observed order of field magnitude. Here, we present a breakthrough by using a multigrid-based general relativistic code, Gmunu, to dynamically simulate the oscillations of highly magnetized non-rotating axisymmetric neutron stars with field strengths of $10^{15-17}$ G under non-linear perturbations. We extract the eigenfrequencies and eigenfunctions of the excited oscillation modes and preliminary results show that the eigenfrequencies decrease with the magnetic to binding energy ratio of the neutron star, implying a suppression of perturbative oscillations in a more magnetized neutron star.
