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Our new study of the two central compact object pulsars, PSR J1210-5226 (P =424 ms) and PSR J1852+0040 (P = 105 ms), leads us to conclude that a weak natalmagnetic field shaped their unique observational properties. In the dipolespin-down formalism, the 2-sigma upper limits on their period derivatives, <2E-16 for both pulsars, implies surface magnetic field strengths of B_s < 3E11G and spin periods at birth equal to their present periods to three significantdigits. Their X-ray luminosities exceed their respective spin-downluminosities, implying that their thermal spectra are derived from residualcooling and perhaps partly from accretion of supernova debris. For sufficientlyweak magnetic fields an accretion disk can penetrate the light cylinder andinteract with the magnetosphere while resulting torques on the neutron starremain within the observed limits. We propose the following as the origin ofradio-quiet CCOs: the magnetic field, derived from a turbulent dynamo, isweaker if the NS is formed spinning slowly, which enables it to accrete SNdebris. Accretion excludes neutron stars born with both B_s < 1E11 G and P >0.1 s from radio pulsar surveys, where such weak fields are not encounteredexcept among very old (> 40 Myr) or recycled pulsars. We predict that thesebirth properties are common, and may be attributes of the youngest detectedneutron star, the CCO in Cassiopeia A, as well as an undetected infant neutronstar in the SN 1987A remnant. In view of the far-infrared light echo discoveredaround Cas A and attributed to an SGR-like outburst, it is especially importantto determine via timing whether Cas A hosts a magnetar or not. If not amagnetar, the Cas A NS may instead have undergone a one-time phase transition(corequake) that powered the light echo.

CCO Pulsars as Anti-Magnetars: Evidence of Neutron Stars Weakly Magnetized at Birth