Detection of precessing circumpulsar disks
arXiv:1406.2935 · doi:10.1093/mnras/stw1057
Abstract
Experimental evidences indicate that formations of disks and planetary systems around pulsars are allowed. Unfortunately, direct detections through electromagnetic observations appear to be quite rare. In the case of PSR 1931+24, the hypothesis of a rigid precessing disk penetrating the pulsar light cylinder is found consistent with radio transient observations from this star. Disk self-occultation and precession may limit electromagnetic observations. Conversely, we show here that gravitational waves generated by disk precessing near the light cylinder of young and middle aged pulsars would be detected by future space interferometers with sensitivities like those expected for DECIGO (DECI-hertz Interferometer Gravitational Wave Observatory) and BBO (Big Bang Observer). The characteristics of circumpulsar detectable precessing disks are estimated as a function of distance from the Solar System. Speculations on upper limits to detection rates are presented.
10 pages,6 figures
References in corpus (10)
- Observation of Gravitational Waves from a Binary Black Hole Merger
- The Parkes multibeam pulsar survey: VI. Discovery and timing of 142 pulsars and a Galactic population analysis
- A Debris Disk Around An Isolated Young Neutron Star
- Interpretation of AMS-02 electrons and positrons data
- The fate of fallback matter around newly born compact objects
- A Cosmic Ray Positron Anisotropy due to Two Middle-Aged, Nearby Pulsars?
- On the pulse--width statistics in radio pulsars. I. Importance of the interpulse emission
- Subtraction-noise projection in gravitational-wave detector networks
- Constraints on Galactic Intermediate Mass Black Holes
- Formation of Sub-millisecond Pulsars and Possibility of Detection