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Journal Article

Search method for long-duration gravitational-wave transients from neutron stars

MPS-Authors
http://pubman.mpdl.mpg.de/cone/persons/resource/persons40534

Prix,  Reinhard
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons40524

Giampanis,  Stefanos
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons42125

Messenger,  Christopher
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

1104.1704.pdf
(Preprint), 907KB

PRD84_023007.pdf
(Any fulltext), 825KB

Supplementary Material (public)
There is no public supplementary material available
Citation

Prix, R., Giampanis, S., & Messenger, C. (2011). Search method for long-duration gravitational-wave transients from neutron stars. Physical Review D, 84(2): 023007. doi:10.1103/PhysRevD.84.023007.


Cite as: http://hdl.handle.net/11858/00-001M-0000-000F-06C4-4
Abstract
We introduce a search method for a new class of gravitational-wave signals, namely long-duration O(hours - weeks) transients from spinning neutron stars. We discuss the astrophysical motivation from glitch relaxation models and we derive a rough estimate for the maximal expected signal strength based on the superfluid excess rotational energy. The transient signal model considered here extends the traditional class of infinite-duration continuous-wave signals by a finite start-time and duration. We derive a multi-detector Bayes factor for these signals in Gaussian noise using $\F$-statistic amplitude priors, which simplifies the detection statistic and allows for an efficient implementation. We consider both a fully coherent statistic, which is computationally limited to directed searches for known pulsars, and a cheaper semi-coherent variant, suitable for wide parameter-space searches for transients from unknown neutron stars. We have tested our method by Monte-Carlo simulation, and we find that it outperforms orthodox maximum-likelihood approaches both in sensitivity and in parameter-estimation quality.