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

TL;DR

This study confirms that certain young neutron stars called CCOs have extremely weak magnetic fields, challenging previous assumptions and revealing complex surface temperature and magnetic structures.

Contribution

First direct measurements of magnetic fields in multiple CCOs, confirming their status as anti-magnetars with weak dipole fields and revealing complex surface magnetic features.

Findings

CCOs have exceptionally weak dipole magnetic fields (~10^10 G)

Surface temperature distributions suggest strong crustal magnetic fields

Spectral features modulated with rotation may be due to cyclotron processes

Abstract

Using XMM-Newton and Chandra, we measure period derivatives for the second and third known pulsars in the class of Central Compact Objects (CCOs) in supernova remnants, proving that these young neutron stars have exceptionally weak dipole magnetic field components. For the 112 ms PSR J0821-4300 in Puppis A, Pdot = (9.28 +/- 0.36)E-18. Its proper motion, mu = 61 +/- 9 mas/yr, was also measured using Chandra. This contributes a kinematic term to the period derivative via the Shklovskii effect, which is subtracted from Pdot to derive dipole Bs = 2.9E10 G, a value similar to that of first measured CCO PSR J1852+0040 in Kes 79, which has Bs = 3.1E10 G. Antipodal surface hot spots with different temperatures and areas are deduced from the X-ray spectrum and pulse profiles. Paradoxically, such nonuniform surface temperature appears to require strong crustal magnetic fields, probably toroidal or quadrupolar components much stronger than the external dipole. A spectral feature, consisting of either an emission line at approximately 0.75 keV or absorption at approximately 0.46 keV, is modulated in strength with the rotation. It may be due to a cyclotron process in a magnetic field on the surface that is slightly stronger than the dipole deduced from the spin-down. We also timed anew the 424 ms 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 is compatible with a cyclotron resonance interpretation of its prominent absorption line at 0.7 keV and harmonics. These results deepen the mystery of the origin and evolution of CCOs: why are their numerous descendants not evident?