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Using XMM-Newton and Chandra, we measure period derivatives for the secondand third known pulsars in the class of Central Compact Objects (CCOs) insupernova remnants, proving that these young neutron stars have exceptionallyweak dipole magnetic field components. For the 112 ms PSR J0821-4300 in PuppisA, Pdot = (9.28 +/- 0.36)E-18. Its proper motion, mu = 61 +/- 9 mas/yr, wasalso measured using Chandra. This contributes a kinematic term to the periodderivative via the Shklovskii effect, which is subtracted from Pdot to derivedipole Bs = 2.9E10 G, a value similar to that of first measured CCO PSRJ1852+0040 in Kes 79, which has Bs = 3.1E10 G. Antipodal surface hot spots withdifferent temperatures and areas are deduced from the X-ray spectrum and pulseprofiles. Paradoxically, such nonuniform surface temperature appears to requirestrong crustal magnetic fields, probably toroidal or quadrupolar componentsmuch stronger than the external dipole. A spectral feature, consisting ofeither an emission line at approximately 0.75 keV or absorption atapproximately 0.46 keV, is modulated in strength with the rotation. It may bedue to a cyclotron process in a magnetic field on the surface that is slightlystronger than the dipole deduced from the spin-down. We also timed anew the 424ms PSR J12010-5226, resolving previous ambiguities about its spin-down rate.Its Pdot = (2.22 +/- 0.02)E-17, corresponding to Bs = 9.8E10 G. This iscompatible with a cyclotron resonance interpretation of its prominentabsorption line at 0.7 keV and harmonics. These results deepen the mystery ofthe origin and evolution of CCOs: why are their numerous descendants notevident?

The Spin-down of PSR J0821-4300 and PSR J1210-5226: Confirmation of Central Compact Objects as Anti-Magnetars