Beating the spin-down limit on gravitational wave emission from the Vela pulsar
Abadie, J. and Lockerbie, N. A. and Tokmakov, K. V., LIGO Scientific Collaboration, Virgo Collaboration (2011) Beating the spin-down limit on gravitational wave emission from the Vela pulsar. Astrophysical Journal, 737 (2). ISSN 1538-4357 (https://doi.org/10.1088/0004-637X/737/2/93)
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Abstract
We present direct upper limits on continuous gravitational wave emission from the Vela pulsar using data from the Virgo detector's second science run. These upper limits have been obtained using three independent methods that assume the gravitational wave emission follows the radio timing. Two of the methods produce frequentist upper limits for an assumed known orientation of the star's spin axis and value of the wave polarization angle of, respectively, 1.9 x 10(-24) and 2.2 x 10(-24), with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of 2.1 x 10(-24), with 95% degree of belief. These limits are below the indirect spin-down limit of 3.3 x 10(-24) for the Vela pulsar, defined by the energy loss rate inferred from observed decrease in Vela's spin frequency, and correspond to a limit on the star ellipticity of similar to 10(-3). Slightly less stringent results, but still well below the spin-down limit, are obtained assuming the star's spin axis inclination and the wave polarization angles are unknown.
ORCID iDs
Abadie, J., Lockerbie, N. A. ORCID: https://orcid.org/0000-0002-1678-3260 and Tokmakov, K. V. ORCID: https://orcid.org/0000-0002-2808-6593;-
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Item type: Article ID code: 39867 Dates: DateEvent20 August 2011PublishedNotes: J. Abadie et al 2011 ApJ 737 93. © 2011. The American Astronomical Society Subjects: Science > Physics > Solid state physics. Nanoscience Department: Faculty of Science > Physics Depositing user: Pure Administrator Date deposited: 30 May 2012 14:27 Last modified: 04 Oct 2024 00:19 Related URLs: URI: https://strathprints.strath.ac.uk/id/eprint/39867