| Abstract : | Based on the studies, progenitors of some of the long gamma-ray bursts (lGRBs) and stripped-envelope supernovae (SESNe) could be narrowed down to massive stars that have stripped their Hydrogen and Helium envelopes, have high spin, and low metallicity. In the past two decades, the most exciting aspects of this field are (i) the correlation of some of the lGRBs with SESNe (ii) Fermi-LAT observed GeV emission in case of some of the lGRBs and their correlation with lower-energy X-ray/Gamma-ray emissions. Till now, for nearly two dozen of lGRBs, the SNe signatures have been detected in the afterglow as a red bump in their late-time light curves.
It is evident that only a tiny fraction (~1%) of SESNe produce broad-lined Ic SNe, which can also display detectable lGRBs. Superluminous SN 2011kl is the only known case so far associated with the ultra-long GRB (ulGRB), e.g., GRB 111209A, and hints that some of these SLSNe I may also be connected with lGRBs. During such energetic explosions, radio-active iron-peaked nuclei are synthesized either by the neutrino wind emitted by the accretion disc or by a cocoon of material surrounding the jet as it pierces through the progenitor star. Another exciting aspect is that the host galaxies of lGRBs are similar to those of SLSNe I in terms of stellar mass, star formation rate, and metallicity, whereas statistically distinct to the host galaxies of normal SNe Ibc. So, the study of lGRBs and associated SNe/SLSNe will add value to the present understanding of the nature of their environment and their explosion mechanisms. If I get a chance to deliver a talk, I would like to speak about the possible physical mechanisms of some of the lGRB-SESNe connection cases observed with the 3.6m-DOT operated by the ARIES. |
