Radio pulsars as progenitors of AXPs and SGRs: magnetic field evolution through pulsar glitches
نویسندگان
چکیده
Glitches are common phenomena in pulsars. After each glitch, there is often a permanent increase in the pulsar’s spin-down rate. Therefore a pulsar’s present spin-down rate may be much higher than its initial value and the characteristic age of a pulsar based on its present spin-down rate and period may be shorter than than its true age. At the same time, the permanent increase of its spindown rate implies that the pulsar’s surface magnetic field is increased after each glitch. Consequently after many glitches some radio pulsars may evolve into the magnetars, i.e., strongly magnetized and slowly rotating neutron stars. Subject headings: pulsars: general—pulsars: individual (PSR B1757-24, Crab, Vela, AXP, SGR)
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