1202.1123 (Shuang-Nan Zhang et al.)
Shuang-Nan Zhang, Yi Xie
We model the evolution of the magnetic fields of neutron stars as consisting
of a long term power-law decay modulated by short term small amplitude
oscillations. Our model predictions on the timing noise $\ddot\nu$ of neutron
stars agree well with the observed statistical properties and correlations of
normal radio pulsars. Fitting the model predictions to the observed data, we
found that their initial parameter implies their initial surface magnetic
dipole magnetic field strength ~ 5E14 G at ~0.4 year old and that the
oscillations have amplitude between E-8 to E-5 and period on the order of
years. For individual pulsars our model can effectively reduce their timing
residuals, thus offering the potential of more sensitive detections of
gravitational waves with pulsar timing arrays. Finally our model can also
re-produce their observed correlation and oscillations of the second derivative
of spin frequency, as well as the "slow glitch" phenomenon.
View original:
http://arxiv.org/abs/1202.1123
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