An accretion disk model for periodic timing variations of pulsars

@article{Qiao2003AnAD,
  title={An accretion disk model for periodic timing variations of pulsars},
  author={Guo-jun Qiao and Y. Q. Xue and Renxin Xu and H. T. G. Wang and Bo-Wen Xiao},
  journal={Astronomy and Astrophysics},
  year={2003},
  volume={407}
}
The long term, highly periodic and correlated variations in both the pulse shape and the rate of slow down of two isolated pulsars (PSRs) PSR B1828 11 and PSR B1642 03 were discovered recently. This phenomenon may provide evidence for "free precession" as suggested in the literature. Some authors presented various kinds of models to explain this phenomenon within the framework of free precession. Here we present an accretion disk model for this precession phenomenon instead. Under reasonable… 

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References

SHOWING 1-10 OF 21 REFERENCES
Evidence for free precession in a pulsar
TLDR
The discovery of long-term, highly periodic and correlated variations in both the pulse shape and the rate of slow-down of the pulsar PSR B1828-11, probably resulting from precession of the spin axis caused by an asymmetry in the shape ofThe pulsar.
An Accretion Model for Anomalous X-Ray Pulsars
We present a model for the anomalous X-ray pulsars (AXPs) in which the emission is powered by accretion from a fossil disk, established from matter falling back onto the neutron star following its
An analysis of the precession of the accretion disk of Hercules X-1
Hercules X-1 exhibits a 35 day cycle in its X-ray intensity and 1.24 s and 1.7 day periodicities in its pulsar rotation and orbit, respectively. The features of the 35 day clock and the presence of a
Precession interpretation of the isolated pulsar psr b1828-11
Pulse timing of the isolated pulsar PSR B1828-11 shows strong Fourier power at periods 1000, 500, and 250 days, correlated with changes in the pulse profile (Stairs, Lyne, & Shemar). We study the
Disk-assisted Spin-down of Young Radio Pulsars
We present a model for the spin-down of young radio pulsars in which the neutron star loses rotational energy not only by emitting magnetic dipole radiation but also by torquing a surrounding disk
Evidence for Free Precession in the Pulsar B1642-03
We present an analysis of the timing data of the pulsar B1642-03, collected over a span of 30 years between 1969 and 1999. During this interval, the timing residuals exhibit cyclical changes with
Free Precession in Quasi-periodic Oscillators
The recent discoveries of quasi-periodic oscillations (QPOs) brought about a surge of theoretical work concerned with the disk-magnetosphere boundary in accreting neutron stars. Much of the detailed
Disk-driven precession in SS 433
We show that a moderately massive disk (10/sup -5/--10/sup -2/ M/sub sun/) can cause the Lense-Thirring precession of the compact object (neutron star or black hole) at its center. The inner regions
PSR 1259-63 : a binary radio pulsar with a Be star companion
The discovery of the first known radio pulsar with a massive, nondegenerate companion is reported. PSR 1259-63, found during a large-scale high-frequency survey of the southern Galactic plane, has a
Radio Pulsar Death Line Revisited: Is PSR J2144-3933 Anomalous?
TLDR
It is found that the inverse Compton scattering-induced space-charge-limited flow model can sustain strong pair production in some long-period pulsars, which allows the newly detected 8.5 s pulsar PSR J2144-3933 to be radio loud without assuming special neutron star equations of state or ad hoc magnetic field configurations.
...
1
2
3
...