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Title:
The Discovery of Rapid X-Ray Oscillations in the Tail of the SGR 1806-20 Hyperflare
Authors:
Israel, G. L.; Belloni, T.; Stella, L.; Rephaeli, Y.; Gruber, D. E.; Casella, P.; Dall'Osso, S.; Rea, N.; Persic, M.; Rothschild, R. E.
Affiliation:
AA(INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone (Rome), Italy ), AB(INAF-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate (LC), Italy ), AC(INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone (Rome), Italy ), AD(School of Physics and Astronomy, Tel Aviv University, 69978 Tel Aviv, Israel; Center for Astrophysics and Space Sciences, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424 ), AE(Eureka Scientific Corporation, 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017 ), AF(INAF-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate (LC), Italy ), AG(INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone (Rome), Italy ), AH(INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone (Rome), Italy; SRON-National Institute for Space Research, Sorbonnelan 2, 3584 CA, Utrecht, Netherlands ), AI(INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, Trieste I-34131, Italy ), AJ(Center for Astrophysics and Space Sciences, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424 )
Publication:
The Astrophysical Journal, Volume 628, Issue 1, pp. L53-L56. (ApJL Homepage)
Publication Date:
07/2005
Origin:
UCP
Astronomy Keywords:
Stars: Pulsars: Individual: Alphanumeric: SGR 1806-20, Stars: Flare, Stars: Neutron, Stars: Oscillations, X-Rays: Bursts
DOI:
10.1086/432615
Bibliographic Code:
2005ApJ...628L..53I

Abstract

We have discovered rapid quasi-periodic oscillations (QPOs) in RXTE/PCA measurements of the pulsating tail of the 2004 December 27 giant flare of SGR 1806-20. QPOs at ~92.5 Hz are detected in a 50 s interval starting 170 s after the onset of the giant flare. These QPOs appear to be associated with increased emission by a relatively hard unpulsed component and are seen only over phases of the 7.56 s spin period pulsations away from the main peak. QPOs at ~18 and ~30 Hz are also detected ~200-300 s after the onset of the giant flare. This is the first time that QPOs are unambiguously detected in the flux of a soft gamma-ray repeater or any other magnetar candidate. We interpret the highest QPOs in terms of the coupling of toroidal seismic modes with Alfvén waves propagating along magnetospheric field lines. The lowest frequency QPO might instead provide indirect evidence on the strength of the internal magnetic field of the magnetar.
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