At the time when the giant flare of SGR1806-20 occurred, the AURIGA ‘‘bar’’ gravitational-wave (GW) detector was on the air with a noise performance close to stationary Gaussian. This allows us to set relevant upper limits, at a number of frequencies in the vicinities of 900 Hz, on the amplitude of the damped GW wave trains, which, according to current models, could have been emitted, due to the excitation of normal modes of the star associated with the peak in x-ray luminosity.
Upper limits on gravitational-wave emission in association with the 27 Dec 2004 giant flare of SGR1806-20 / Baggio, L.; Bignotto, M.; Bonaldi, M.; Cerdonio, M.; Conti, L.; De Rosa, M.; Falferi, P.; Fortini, P.; Inguscio, M.; Liguori, N.; Marin, F.; Mezzena, R.; Mion, A.; Ortolan, A.; Prodi, G. A.; Poggi, S.; Salemi, F.; Soranzo, G.; Taffarello, L.; Vedovato, G.; Vinante, A.; Vitale, S.; Zendri, J. P.. - In: PHYSICAL REVIEW LETTERS. - ISSN 0031-9007. - 95:8(2005), pp. 1-4. [10.1103/PhysRevLett.95.081103]
Upper limits on gravitational-wave emission in association with the 27 Dec 2004 giant flare of SGR1806-20
Salemi, F.;
2005
Abstract
At the time when the giant flare of SGR1806-20 occurred, the AURIGA ‘‘bar’’ gravitational-wave (GW) detector was on the air with a noise performance close to stationary Gaussian. This allows us to set relevant upper limits, at a number of frequencies in the vicinities of 900 Hz, on the amplitude of the damped GW wave trains, which, according to current models, could have been emitted, due to the excitation of normal modes of the star associated with the peak in x-ray luminosity.| File | Dimensione | Formato | |
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