Abstract
We propose a theoretical model for magnetar giant flare to explain the flaring activity on 2004 December 27 from SGR1806-20 comprehensively. A global rearrangement is expected by the magnetic reconnection that requires explaining the giant SGR flares. In this paper we propose two regions of flares: preflare on the surface of magnetar and main burst at a distance of light cylinder radius. Acquiring the maximum potential drop on the magnetar surface, adopting space charge limited flow model, and using magnetic field B ≈ 1015 G, the luminosities of flare energies release for the preflare phase and main burst phase are found to be in the order of 1041 erg·sˉ1 and 1044 erg·sˉ1 respectively, conforming to magnetar burst energy and flare temperature is determined by considering black body radiation.
Highlights
Soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been identified as isolated superstrong magnetized neutron stars—magnetars
Acquiring the maximum potential drop on the magnetar surface, adopting space charge limited flow model, and using magnetic field B ≈ 1015 G, the luminosities of flare energies release for the preflare phase and main burst phase are found to be in the order of 1041 erg·s−1 and 1044 erg·s−1 respectively, conforming to magnetar burst energy and flare temperature is determined by considering black body radiation
The goal of this paper is to investigate the flare energy release for pre flare phase and main flare phase at a height of 106 cm and 1010 cm from the stellar centre for the duration of 1.0 second and 0.1 second respectively as our model is confined within the closed magnetic field lines on the basis of giant flare on 2004 December 27 from SGR1806-20
Summary
Soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been identified as isolated superstrong magnetized neutron stars—magnetars. It is expected that twisted field lines [5] in the magnetosphere could relax by reconnection & release energy which we could observe as SGR bursts. With reservation for our understanding of reconnection and particle acceleration, we propose here that the bursting activity of SGRs is due to the reconnection-type events in which magnetic energy stored in the non potential (current carrying) magnetic field is released in the magnetosphere. In contrast to the common short burst, giant flare with enormous energy and long bursting duration is exceptionally observed from SGRs. In the space-charge limited flow (SCLF) model, it is assumed that particles are not bound to the neutron star surface by ionic bonding, but instead are freely available.
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