Measuring the Magnetic Fields of Central Compact Objects in Supernova Remnants

Details Measuring the Magnetic Fields of Central Compact Objects in Supernova Remnants Measuring the Magnetic Fields of Central Compact Objects in Supernova Remnants

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007xmm..prop...23h&link_type=abstract

XMM-Newton Proposal ID #05506701

Physics

Supernovae, Supernova Remnants, Diffuse (Galactic) Emission And Isolated Neutron Stars, Psr J1852+0040, Xmm-Newton Proposal Id #05506701

Scientific paper

X-ray timing studies of two X-ray pulsars in SNRs have detected no braking of their rotation, implying upper limits of 3E11 G on their surface dipole fields, well below those of ordinary young pulsars. We proposed that weak B-fields related to slow natal spin may be the physical basis of the class of Central Compact Objects (CCOs), including the unseen pulsar in SN 1987A. This proposal leverages existing timing data on CCO pulsars to determine if they are spinning down and, if so, to measure their magnetic fields by obtaining coherent timing solutions linking all previous data. Fields as small as 1E10 G can be measured in this way. Alternatively, accretion of supernova debris through a fallback disk may be occurring, which would be detectable as torque noise.

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