Dynamical Flattening of Crust, Fluid Outer Core and Solid Inner Core for PSR B1828-11

Details Dynamical Flattening of Crust, Fluid Outer Core and Solid Inner Core for PSR B1828-11 Dynamical Flattening of Crust, Fluid Outer Core and Solid Inner Core for PSR B1828-11

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...6e..11k&link_type=abstract

Neutron Stars and Black Holes in Star Clusters, 26th meeting of the IAU, Joint Discussion 6, 17-18 August 2006, Prague, Czech Re

Physics

Scientific paper

An investigation of rotation variations allows studying a structure of a neutron star. Analysis of the time-of-arrival (TOA) pulses fluctuations can be reflection of thin effects of neutron stars rotational dynamics. In observations of radiation from some pulsars: PSR 2217+47, PSR 0531+21, PSR B0833-45, PSR B1828-11, PSR B1642-03 a long periodic fluctuations of TOA pulses with period from 25 to 6136 days were detected. PSR B1828-11 has long-term, highly periodic and correlated variations pulse shape and of the rate of slow-down with period variations approximately 1000, 500, 250 and 167 days. TOA variations of pulsars can be interpreted by three reasons: gravitational perturbation by planetary bodies, peculiarities of a pulsar interior like Tkachenko oscillations and free precession motion, when axis of rotation do not coincide with vectors of the angular moment of solid crust, liquid outer core and crystal core. We use the Hamiltonian canonical method of Getino for the dynamically symmetrical three-layer model of the pulsar PSR B1828-11. We explane four harmonics of pulses variations as precessions and nutations of a neutron star owing to differential rotation of crust, fluid outer core (FOC) and solid inner core (SIC) by Chandler wobble (CW), Inner Chandler Wobble (ICW), Free Core Nutation (FCN) and Free Inner Core Nutation (FICN). We have got the estimates of dynamical flattening of the crust, the FOC and the SIC of the pulsar (~10^-9) for known periodic variations of the TOA pulse from PSR B1828-11: P[CW] = 167 days, P[ICW] = 500 days, P[FCN] = 250 days, P[FICN] = 1000 days. With increase of pulsar radius on 1.1 km the dynamical flattening of crust grows in 5.5 times, and flattening of fluid outer core increases only in 1.5 times. Changing of the radius of the inner core (from 0.6 to 1.1 km) almost does not influence to dynamical flattening of the solid inner core. We have estimates the flateness of crust ~ 0.3 · 10^-9, flateness of FOC ~ 0.6 · 10^-9 and flateness of SIC is ~ 4.7 · 10^-9. We have offered the realistic model of the dynamical pulsar structure and two explanations of the feature of flattening of the crust, the outer fluid core and the inner solid core of the pulsar.

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