Upper limits on gravitational-wave emission in association with the 27 dec 2004 giant flare of SGR1806-20

Year: 2005

Authors: 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.

Autors Affiliation: Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Bhiba, 277-8582, Japan;
INFN Padova Section and Departmento of Physics, 35131 Padova, Italy;
Istituto di Fotonica e Nanotecnologie CNR-ITC and INFM Gruppo Collegato di Trento, Padova Section, 38050 Povo (Trento) Italy;
CNR – Istituto Nazionale di Ottica Applicata, 80078 Pozzuoli (NA) Italy;
INFN Firenze Section, 50121 Firenze, Italy;
Physics Department, University of Ferrara and INFN Ferrara Section, 44100 Ferrara, Italy;
LENS and Physics Department, University of Firenze, 50121 Firenze, Italy;
Physics Department, University of Trento, 38050 Povo (Trento) Italy;
INFN, Laboratori Nazionali di Legnaro, 35020 Legnaro (Padova) Italy;
INFN Padova Section, 35100 Padova, Italy

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.


Volume: 95 (8)      Pages from: 081103-1  to: 081103-4

KeyWords: Gravitational-wave (GW) detector; Gravitational-wave emission; X-ray luminosity, Acoustic waves; Gravitational effects; X rays, Acoustic emissions
DOI: 10.1103/PhysRevLett.95.081103

Citations: 23
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