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| Paper: |
Rebrightening in GRBs by Precessing Jet |
| Volume: |
312, Third Rome Workshop on Gamma-Ray Bursts in the Afterglow Era |
| Page: |
423 |
| Authors: |
Fargion, D. |
| Abstract: |
A clear gamma polarization in the γ signals from GRB021206 probes the presence of a very thin collimated jet (opening angle Δθ ≤ 0.6°; ΔΩ/Ω ≤ 2.5 · 10−5) in Gamma Ray Burst, GRBs. The last and well proved GRB030329/SN2003dh time and space coincidence confirms definitely the earliest GRB980425/SN1998bw connection among GRB and Supernova. The apparent extreme GRBs luminosity is just the extreme beamed blazing gamma Jet observed in axis during a supernova birth. The maximal isotropic SN power, dESN/dt ≈ 1045 erg s−1, because of its probably energy equi-partition, should be collimated even into an even thinner jet ΔΩ/Ω ≤ 10−8, in order to explain at once the apparent observed maximal GRBs output, dEGRB/dt ≈ dESN/dt Ω/ΔΩ ≈ 1053 erg s−1. Consequently one-shoot thin Jet GRBs needs many more dNGRB/dt ≈ Ω/ΔΩ · dNFireball/dt event rate than any spread isotropic Fireballs. Such a rate exceeds even the known Supernova one. To overcome the puzzle a persistent precessing decaying jet (life-time τJet ≥ 103 τGRB) is compelling. The late relic GRBs sources may be found in compact SNRs core, as NS or BH jets; at much later epoch, their lower power γ jets may be within detectablility only from nearby galactic distances, as Soft Gamma Repeaters (SGRs) or anomalous X-ray Pulsars, AXPs. This common Jet nature explains some connection between GRBs and SGRs spectra. The geometrical multi-precessing beaming and their reappearance to the observer may explain the puzzling presence of X-Ray precursors in GRBs as well as in SGRs. A mysterious re-brightening afterglows observed in early and late GRB030329 optical transient, like in the 27 August 1998 and 18 April 2001 SGRs 1900 + 14 events, might be understood as the damped oscillatory imprint left by such a multi-precessing γ-X-Optical and Radio Jet. |
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