Search for Gravitational Waves Associated with the August 2006 Timing Glitch of the Vela Pulsar

Authors

J. Abadie, California Institute of Technology
B. P. Abbott, Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
R. Abbott, University of Wisconsin-Milwaukee
R. Adhikari, Stanford University
P. Ajith, Louisiana State University
B. Allen, University of Florida
G. Allen, University of Birmingham
E. Amador Ceron, Leibniz University Hannover
R. S. Amin, Montana State University
S. B. Anderson, LIGO
W. G. Anderson, University of Glasgow
M. A. Arain, University of Western Australia
M. Araya, Massachusetts Institute of Technology
Y. Aso, Columbia University
S. Aston, University of Texas at Brownsville
P. Aufmuth, University of Melbourne
C. Aulbert, San Jose State University
S. Babak, Lomonosov Moscow State University
P. Baker, Pennsylvania State University
S. Ballmer, Washington State University Pullman
D. Barker, University of Oregon
B. Barr, LIGO
P. Barriga, Syracuse University
L. Barsotti, University of Maryland
M. A. Barton, University of Massachusetts
I. Bartos, University of Mississippi
R. Bassiri, NASA Goddard Space Flight Center
M. Bastarrika, Charles Sturt University
B. Behnke, Carleton College
M. Benacquista, Australian National University
Shaon Ghosh, Montclair State UniversityFollow

Document Type

Article

Publication Date

2-1-2011

Journal / Book Title

Physical Review D

Abstract

The physical mechanisms responsible for pulsar timing glitches are thought to excite quasinormal mode oscillations in their parent neutron star that couple to gravitational-wave emission. In August 2006, a timing glitch was observed in the radio emission of PSR B0833-45, the Vela pulsar. At the time of the glitch, the two colocated Hanford gravitational-wave detectors of the Laser Interferometer Gravitational-wave observatory (LIGO) were operational and taking data as part of the fifth LIGO science run (S5). We present the first direct search for the gravitational-wave emission associated with oscillations of the fundamental quadrupole mode excited by a pulsar timing glitch. No gravitational-wave detection candidate was found. We place Bayesian 90% confidence upper limits of 6.3×10-21 to 1.4×10 -20 on the peak intrinsic strain amplitude of gravitational-wave ring-down signals, depending on which spherical harmonic mode is excited. The corresponding range of energy upper limits is 5.0×1044 to 1.3×1045erg.

DOI

10.1103/PhysRevD.83.042001

MSU Digital Commons Citation

Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya, M.; Aso, Y.; Aston, S.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; and Ghosh, Shaon, "Search for Gravitational Waves Associated with the August 2006 Timing Glitch of the Vela Pulsar" (2011). Department of Physics and Astronomy Faculty Scholarship and Creative Works. 112.
https://digitalcommons.montclair.edu/physics-astron-facpubs/112

Published Citation

Abadie, J., Abbott, B. P., Abbott, R., Adhikari, R., Ajith, P., Allen, B., ... & Giardina, K. D. (2011). Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar. Physical Review D, 83(4), 042001.