Solving Grbs and Sgrs Puzzles by Precessing Jets Wspc -proceedings Trim Size: 9in X 6in Fargion-ol-or2

A persistent, thin micro-nano sr beamed gamma jet may be ejected from BH and Pulsars, powered by ultra-relativistic electron pairs. These precessing and spinning γ jet 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 the thin jet explains naturally the observed erratic multi-explosive structure of different GRBs. The jets are precessing (by binary companion or inner asymmetry) and decaying on time scales of a few hours but they usually keep staying inside the observer cone view only few seconds duration times (GRB); the jets whole lifetime, while decaying in output, could survive as long as thousands of years, linking huge GRB-SN jet apparent Luminosity to more modest SGR relic Jets (at corresponding X-Ray pulsar output). 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 the 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 the largest cosmic volumes. The most beamed the hardest. On the contrary, the nearer ones, within tens Mpc distances, are mostly observable on the cone jet periphery. Their consequent large impact crossing angle leads to longest anomalous SN-GRB duration, with lowest fluency and the softest spectra, as in earliest GRB98425 and recent GRB060218 signature. A majority of GRB jet blazing much later (weeks, months after) may hide their progenitor explosive SN after-glow and therefore they are called orphan GRB. The late law power GRBs are observable as local SGRs (or in outer near extragalactic, XRF) and they are linked to anomalous X-ray AXPs. Conical shape of few nebulae and the pre-cessing jet of few known micro-quasar, describe in space the model signature. Recent outstanding episode of X-ray precursor, ten minutes before the main GRB event, cannot be understood otherwise. 2 Fig. 1. Most Recent Swift GRB isotropic apparent energy 1 versus their observed red-shift in Log-Log plot: earlier GRB020903, GRB030329, GRB031203 and the nearest GRB980425, at redshift …