On the nature of QPO in the tail of SGR giant flares

Details On the nature of QPO in the tail of SGR giant flares On the nature of QPO in the tail of SGR giant flares

2007-06-25

arxiv.org/abs/0706.3698v1

Astrophys.J.680:1398-1404,2008

Astronomy and Astrophysics

Astrophysics

7 pages, 4 figures, emulateapj style

Scientific paper

10.1086/587925

A model is presented for the quasiperiodic component of magnetar emission during the tail phase of giant flares. The model invokes modulation of the particle number density in the magnetosphere. The magnetospheric currents are modulated by torsional motion of the surface and we calculate that the amplitude of neutron star surface oscillation should be ~1% of the NS radius in order to produce the observed features in the power spectrum. Using an axisymmetric analytical model for structure of the magnetosphere of an oscillating NS, we calculate the angular distribution of the optical depth to the resonant Compton scattering. The anisotropy of the optical depth may be why QPO are observed only at particular rotational phases.

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