Statistics – Applications
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0403s&link_type=abstract
American Astronomical Society, HEAD meeting #9, #4.03; Bulletin of the American Astronomical Society, Vol. 38, p.347
Statistics
Applications
Scientific paper
The structure of pulsar magnetosphere has remained a persistent puzzle for almost 40 years. We present the first self-consistent solution of the magnetospheric structure for the most general geometry where pulsar magnetic and rotation axes are misaligned. This 3D time-dependent numerical solution is calculated in the approximation of force-free relativistic MHD. The shape of field lines is asymptotically split-monopolar with a warped equatorial current sheet forming a striped wind. We determine the electromagnetic spin-down energy loss to be L = mu^2 Omega^4/c^3 (1+sin^2(theta)) for a pulsar with dipole moment "mu", frequency "Omega", and magnetic inclination angle "theta". Thus pulsars with larger obliqueness spin down faster and should leave an excess of lower obliqueness pulsars near the death line in P-Pdot diagram. This effect can be seen in the pulsar data. Other applications of the full magnetospheric solution include the interpretation of gamma-ray pulse profiles and time-dependent radio phenomenology.
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