2021/08/02 by Bakır, İrem, Ekşi, Kazım Yavuz
#FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE)
paper · doi:10.48550/arxiv.2108.01051
Some of the young neutron stars, the magnetars, have ultra-strong magnetic fields. The models invoked for the origin of magnetar fields require very specific conditions with extreme parameters, which are incompatible with the inference that the birth rate of magnetars is comparable to the rate of core-collapse supernovae. We propose that these seemingly contradictory trends can be reconciled if both pulsars and magnetars pass through a dynamo process at the proto-neutron star (PNS) stage. We invoke a shear-driven dynamo model for the generation of PNS magnetic fields. We argue that the toroidal fields of central compact objects are shaped by the Ω-effect, even though they do not pass through a genuine dynamo process.