Inner core wobble and free core nutation of pulsar PSR B1828-11

Details Inner core wobble and free core nutation of pulsar PSR B1828-11 Inner core wobble and free core nutation of pulsar PSR B1828-11

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008adspr..42.1391k&link_type=abstract

Advances in Space Research, Volume 42, Issue 8, p. 1391-1397.

Physics

Scientific paper

PSR B1828-11 has long-term, highly periodic and correlated variations in pulse shape and a slow-down rate with period variations of approximately 1000, 500 and 250 days [Stairs, I.H., Lyne, A.G., Shemar, S.L. Evidence for free precession in a pulsar. Nature 406, 484 486, 2000]. There are three potential explanations of pulses time-of-arrival from a pulsar. These are related to the interior of the neutron star, planetary bodies, free precession and nutation. We use the Hamiltonian canonical method of Getino (1995) for analyzing the dynamically symmetric pulsar PSR B1828-11, consisting of a rigid crust, elliptical liquid outer core and solid inner core. Using the theory of differential rotation of a pulsar, we investigate the dependence on Chandler wobble period, inner core wobble, retrograde free core nutation and prograde free inner core nutation from ellipticity of the inner crystal core, outer liquid core and total pulsar.

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