Measuring the Magnetic Field of the CCO Pulsar in Puppis A

Details Measuring the Magnetic Field of the CCO Pulsar in Puppis A Measuring the Magnetic Field of the CCO Pulsar in Puppis A

Sep 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010cxo..prop.2979h&link_type=abstract

Chandra proposal ID #12500003

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Scientific paper

Having discovered the pulsar in Puppis A and ruled out a magnetar, we will determine if it is a weakly magnetized neutron star like the other CCO pulsars by obtaining a phase-coherent timing solution, the only practical way of measuring its spin-down rate. Our sensitivity to P-dot will correspond to a surface dipole B-field as small as 3.e10 G, comparable to our measured value for the CCO pulsar PSR J1852+0040 in Kes 79. New spectra will also allow us to further localize its apparent 0.8 keV emission line in rotation phase, and to model the emission and viewing geometry of this unique system. This will provide important support for the "anti-magnetar" model of CCOs, while exploring possible reasons for their unexplained surface hot spots.

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