Cannonball Model Of Gamma Ray Bursts Research Articles

The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts

In the cannonball model of gamma-ray bursts (GRBs), a highly relativistic jet of plasmoids of ordinary stellar matter that is ejected during stellar collapse or shortly after by fallback matter, produces simultaneously a GRB and a cosmic-ray burst by scattering light and charged particles in its path. This association and the observed knee at ∼1 TeV in the energy spectrum of Galactic cosmic-ray electrons imply a maximum peak energy ∼2.25 MeV in the energy spectrum of GRBs in the 1 keV–10 MeV band. Such a peak energy and the Amati correlation in GRBs imply a maximum isotropic equivalent energy release of ∼3.8 × 1054 erg in GRBs, in the 1 keV–10 MeV band. Both predictions are in good agreement with up-to-date observations.

On The Origin of Supernova-less Long Gamma-Ray Bursts

Abstract The fraction of long duration gamma-ray bursts (GRBs) without an associated bright supernova (SN-less GRBs) at low redshifts is comparable to that of GRBs associated with bright supernovae (SN-GRBs). The prompt emission and its fast decline phase in both types of GRBs are well described by the cannonball model of GRBs, where inverse Compton scattering of ambient light is the dominant γ-ray production mechanism. However, in SN-less GRBs, the fast decay of the prompt emission appears to be overtaken by an afterglow powered by a millisecond pulsar, while, in SN-GRBs, the late-time X-ray afterglow is well described by synchrotron radiation from the decelerating jet in the interstellar medium. We use their different X-ray light curves to determine the ratio of SN-less GRBs/SN-GRBs at very high redshifts. We find that at z > 4, this ratio is the same as that at small redshifts. Such a z-independent ratio suggests that the origin of SN-less GRBs is a phase transition of neutron stars to quark stars in high-mass X-ray binaries, rather than the merger of neutron stars.

Conical fireballs, cannonballs, and jet breaks in the afterglows of gamma ray bursts

The 'jet-break' in the X-ray afterglow of gamma ray bursts (GRBs) appears to be correlated to other properties of the X-ray afterglow and the prompt gamma ray emission, but the correlations are at odds with those predicted by the conical fireball model of GRBs. The correlations are in good agreement, however, with those predicted by the Cannonball model of GRBs.

ON THE EVOLUTION OF THE SPECTRAL BREAK IN THE AFTERGLOW OF GAMMA-RAY BURSTS

The temporal evolution of the spectral break in the time resolved spectral energy density of the broad band afterglow of gamma ray bursts (GRBs) 091127 and 080319B was shown recently to be inconsistent with that expected for the cooling break in the standard fireball model of GRBs. Here we show that it is, however, in good agreement with the predicted temporal evolution of the smooth injection break/bend in the cannonball model of GRBs.

On the "Canonical Behavior" of the X-Ray Afterglows of Gamma-Ray Bursts Observed with Swift 's XRT

The "canonical behaviour" of the early X-ray afterglows of long-duration Gamma-Ray Bursts (GRBs) --observed by the X-Ray Telescope of the SWIFT satellite-- is precisely the one predicted by the Cannonball model of GRBs.

Is There a 1998[CLC]bw[/CLC]-like Supernova in the Afterglow of Gamma-Ray Burst 011121?

We use the very simple and successful cannonball model of gamma-ray bursts (GRBs) and their afterglows (AGs) to analyze the observations of the strongly extinct optical AG of the relatively nearby GRB 011121; these observations were made with ground-based telescopes at early times and with the Hubble Space Telescope at later times. We show that GRB 011121 was indeed associated with a 1998bw-like supernova at the GRB's redshift, as we had specifically predicted for this GRB before the supernova could be observed.