Models for the formation of binary and millisecond radio pulsars

摘要: The peculiar combination of a relatively short pulse period and weak surface dipole magnetic field strength binary radio pulsars finds consistent explanation in terms (i) decay the component neutron-star fields on timescale (2–5) × 106 yr, with (ii) spin-up rotation neutron star during subsequent mass-transfer phase. four known appear to fall into two different categories. Two them, PSR 0655 + 64 1913 16, have orbital periods ( 0.7M⊙) white dwarf. Only last-mentioned case is position pulsar close galactic plane natural consequence. In first-mentioned progenitor system most probably was cataclysmic-variable which dwarf collapsed by accretion.