Lower bound on the magnetic field strength of a magnetar from analysis of SGR giant flares

• Published in: Astronomy letters 2011-05, Vol.37 (5), p.332-342
• Main Authors: Gvozdev, A. A., Ognev, I. S., Osokina, E. V.
• Format: Article
• Language: English
• Subjects: Astronomy; Astrophysics and Astroparticles; Emissivity; Energy; Magnetic fields; Neutrinos; Observations and Techniques; Physics; Physics and Astronomy; Radio frequency plasma; Solar flares
• ISSN: 1063-7737; 1562-6873
• DOI: 10.1134/S1063773711040025

Based on the magnetar model, we have studied in detail the processes of neutrino cooling of an electron-positron plasma generating an SGR giant flare and the influence of the magnetar magnetic field on these processes. Electron-positron pair annihilation and synchrotron neutrino emission are shown to make a dominant contribution to the neutrino emissivity of such a plasma. We have calculated the neutrino energy losses from a plasma-filled region at the long tail stage of the SGR 0526-66, SGR 1806–20, and SGR 1900+14 giant flares. This plasma can emit the energy observed in an SGR giant flare only in the presence of a strongmagnetic field suppressing its neutrino energy losses. We have obtained a lower bound on the magnetic field strength and showed this value to be higher than the upper limit following from an estimate of the magnetic dipole losses for the magnetars being analyzed in a wide range of magnetar model parameters. Thus, it is problematic to explain the observed energy release at the long tail stage of an SGR giant flare in terms of the magnetarmodel.