Authors: E.P.J. de Haas
The hypothesis is presented that pulsar-time is geodetic precession rotation time, in both the causal sense and the quantitative sense (T-pulsar exactly equals T-geodetic). The causal sense implies the hypothesis that, in the outer crust of the neutron star, the curvature of the metric favors alignment of elementary particle magnetic moments along the geodetic precession. A consequence of this hypothesis is the partial decoupling of pulsar time and orbital rotation time. For a ``canonical'' neutron star, with 1.4 solar mass and a radius of 10 km, this implies that T-orbit equals approximately one fifth of T-pulsar. The pulsar time as being geodetic precession time explains the extreme stability of pulsar frequencies, despite strong magnetic turbulences. It also quite naturally explains the tilted axis of the neutron stars magnetic moment relative to its orbital axis. The hypothesis is formulated within the environment of the Ehlers-Pirani-Schild Weyl Space Free Fall Grid approach as developed in two previous papers, but it should be theory independent and thus be derivable in GR-Schwarzschild as well.
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