Radio pulsars as progenitors of AXPs and SGRs: magnetic field evolution through pulsar glitches

摘要

Glitches are common phenomena in pulsars. After each glitch, there is usuallya permanent increase in the pulsar's spin-down rate. Therefore a pulsar'spresent spin-down rate may be much higher than its initial value. Thus thecharacteristic age of a pulsar based on its present spin-down rate and periodmay be shorter than a pulsar's age. At the same time, the permanent increase ofits spin-down rate implies that the pulsar's surface magnetic field isincreased after each glitch. Consequently after many glitches some radiopulsars may evolve into AXPs and SGRs, i.e., strongly magnetized and slowlyrotating neutron stars.