Fargion 2006 GRB和SGR的进动模型

主要内容:
Fargion做了很多这方面的工作。

精彩摘抄:


文章信息:

astro-ph/0612319 [abs, ps, pdf, other] :

Title: Solving GRBs and SGRs puzzles by precessing Jets
Authors: D.Fargion, O.Lanciano, P.Oliva
Comments: 10 pages, 16 figures

A persistent, thin, micro-nano sr. beamed gamma jet, may be ejected from BH and Pulsars, powered by ultra-relativistic electron pairs. These jet while precessing and spinning are originated by Inverse Compton and-or Synchrotron Radiation at pulsars or micro-quasars sources. They are most powerful at Supernova birth, blazing, once on axis, to us and flashing GRB detector. The trembling of thin jets explains naturally the observed erratic multi-explosive structure of different GRBs. The jets are precessing and decaying on time scales of a few hours surviving as long as thousands of years, linking huge GRB-SN jet apparent Luminosity to more modest SGR relic Jets. Therefore long-life SGR may be repeating and if they are around our galaxy they might be observed again as the few known ones and a few rarer extragalactic XRFs. The orientation of the beam respect to the line of sight plays a key role in differentiating the wide GRB morphology. The relativistic cone is as small as the inverse of the electron progenitor Lorentz factor. The hardest and brightest gamma spectra are hidden inside the inner gamma jet axis. To observe the inner beamed GRB events one needs the widest SN sample and largest cosmic volumes. The most beamed are hardest.The nearest ones, within tens Mpc distances, are mostly observable on cone jet periphery leading to longest SN-GRB duration, with lowest fluency and the softest spectra, as in earliest GRB98425 and recent GRB 060218 signature. Conical shape of few nebulae describe in space the model signature. Recent X-ray precursor, like in GRB060124, ten minutes before the GRB event, or in SGR1806-20 two minutes before the main giant burst cannot be understood otherwise.