Timing PSR J1852+004 in Supernova Remnant Kes 79: Plan B

Details Timing PSR J1852+004 in Supernova Remnant Kes 79: Plan B Timing PSR J1852+004 in Supernova Remnant Kes 79: Plan B

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007cxo..prop.2389h&link_type=abstract

Chandra Proposal ID #09500297

Computer Science

Chandra Proposal Id #09500297

Scientific paper

Timing of PSR J1852+0040 in SNR Kes 79 has shown no change in its spin period. Its surface B is < 2x10^11 G in the dipole spin-down formalism, unique for a young, rotation-powered pulsar, and incompatible with its X-ray luminosity and pulse properties. Instead, it may be accreting supernova debris, in which case it can remain in a near-equilibrium spin with only random torque noise. We propose to continue our timing of PSR J1852+0040 to measure its P-dot and/or torque noise in order to decide between these models. In any model, PSR J1852+0040 must have a weak magnetic field, which may also explain the class of CCOs, e.g., 1E 1207.4-5209. In those pulsars born spinning slowly, the dynamo may generate a weaker field, which enables it to accrete.

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