Towards a complete theory of gamma-ray bursts

Abstract Gamma ray bursts (GRBs) are notorious for their diversity. Yet, they have a series of common features. The typical energy of their γ -rays is a fraction of an MeV. The energy distributions are well described by a “Band spectrum”, with “peak energies” spanning a surprisingly narrow range. The time structure of a GRB consists of pulses, superimposed or not, rising and decreasing fast. The number of photons in a pulse, the pulses’ widths and their total energy vary within broad but specific ranges. Within a pulse, the energy spectrum softens with increasing time. The duration of a pulse decreases at higher energies and its peak intensity shifts to earlier time. Many other correlations between pairs of GRB observables have been identified. Last (and based on one measured event!) the γ -ray polarization may be very large. A satisfactory theory of GRBs should naturally and very simply explain, among others, all these facts. We show that the “cannonball” (CB) model does it. In the CB model the process leading to the ejection of highly relativistic jetted CBs in core-collapse supernova (SN) explosions is akin to the one observed in quasars and microquasars. The prompt γ -ray emission—the GRB—is explained extremely well by inverse Compton scattering of light in the near environment of the SN by the electrons in the CBs’ plasma. We have previously shown that the CB-model's description of GRB afterglows as synchrotron radiation from ambient electrons—swept in and accelerated within the CBs—is also simple, universal and very successful. The only obstacle still separating the CB model from a complete theory of GRBs is the theoretical understanding of the CBs’ ejection mechanism in SN explosions.