Magnetospheric Emission in Soft Gamma-Ray Repeaters

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Session 5 -- Gamma Ray Astronomy
Display presentation, Monday, June 12, 1995, 9:20am - 6:30pm

[5.05] Magnetospheric Emission in Soft Gamma-Ray Repeaters

M. Fatuzzo (Wesleyan College), F. Melia (University of Arizona)

Recent associations of Soft Gamma-Ray Repeaters (SGR) with supernova remnants strongly suggest that these transient events are produced in young neutron star environments, thereby supporting the view that such bursts are produced when these stars undergo structural adjustments. In previous work, it was shown that the crustal disturbances associated with such structural adjustments would load and energize a neutron star's magnetosphere with an ensuing generation of sheared Alfv\'en waves and subsequently result in a mildly relativistic stellar wind. The structure of the particle efflux was determined and the spectrum of the resulting radiation was calculated, incorporating the key effects due to mildly relativistic magnetic bremsstrahlung, a frequency dependent photospheric radius and angle dependent boosting of the intensity for emitting elements at different inclinations. Here, we extend this study in order to apply our results to the three known SGR sources and thereby determine their underlying physical conditions and their inferred distances. In addition, we determine what observable impact SGR bursts can have on the surrounding plerion environments. Motivated by the similarity between G 10.0-0.3 and the Crab nebula, we consider the possibility that glitching activity on the Crab Pulsar produces SGR-like bursts and determine whether the previously correlated wisp activity can be explained within the framework of our model.

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