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We investigate the effect of strong magnetic fields on the adiabatic radialoscillations of hadronic stars. We describe magnetized hadronic matter withinthe framework of the relativistic nonlinear Walecka model and integrate theequations of relativistic radial oscillations to determine the fundamentalpulsation mode. We consider that the magnetic field increases, in a densitydependent way, from the surface, where it has a typical magnetar value of$10^{15}$ G, to the interior of the star where it can be as large as $3 \times10^{18}$ G. We show that magnetic fields of the order of $10^{18}$ G at thestellar core produce a significant change in the frequency of neutron starpulsations with respect to unmagnetized objects. If radial pulsations areexcited in magnetar flares, they can leave an imprint in the flare lightcurvesand open a new window for the study of highly magnetized ultradense matter.

Properties of strongly magnetized ultradense matter and their imprints on magnetar pulsations