Observational Indications of Free Precession in Radio Pulsars: Update and Progress

Details Observational Indications of Free Precession in Radio Pulsars: Update and Progress Observational Indications of Free Precession in Radio Pulsars: Update and Progress

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr4a4001s&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Isolated radio pulsars typically "spin down" in a more-or-less regular fashion, with young pulsars often showing some modulation from stochastic timing noise or glitches. PSR B1828-11 is a young, isolated pulsar which shows strong, harmonically related periodicities with a fundamental period of about 1000 days in its timing residuals relative to a simple spin-down law. These rotational periodicities are strongly correlated with variations in the pulse shape. The most natural explanation for the related phenomena is free precession of the neutron star, though traditional theories of vortex pinning predict that such precession should not be possible on the observed timescales. We are now acquiring high-resolution observations with which we are studying the pulse beam shape and polarization at different precessional phases in order to infer and detect changes in geometry. This will allow us to check the beam-shape model of Link and Epstein (2001) and possibly to determine whether the true fundamental of the precession is 500 or 1000 days.

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