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Gamma Ray Bursts (GRBs) are the highest energy transient events in the universe. GRBs emit photons in MeV to GeV energy range that lasts for a few seconds to minutes, and in rare cases, even hours. Phenomenologically, GRBs are emitted from highly collimated jets produced in catastrophic astrophysical events such as Type Ic Supernova or compact object mergers (NS-NS or NS-BH merger) producing total energy in the range 1.0e51-1.0e53 ergs. GRBs represent the earliest detectable signatures of these explosive events in the electromagnetic spectrum. However, due to the collimated nature of the jets, detecting GRBs is highly probabilistic. Meanwhile, non-detection can also give insights into the geometries of the associated explosive event. A faster GRB transient is followed by a longer lasting (~few years to decades) electromagnetic emission in X-ray to Radio band, called the Afterglow. Together, GRB and its afterglow provide multi-band data to investigate the various properties of the associated explosion and form a strong stakeholder in multi-messenger astronomical studies. Although very prevalent, the basic theoretical framework for Gamma Ray Bursts remains highly debated. In recent years, events such as GW170817/GRB170817A (NS-NS merger), GRB221009A (aka BOAT, Brightest of All Time), and GRB031203 (and other similar low luminous GRB) have further challenged our existing knowledge of GRBs. In this talk, I will present a brief overview of the GRB Zoo and the physics behind it. Following this, I will discuss our attempt towards a unified GRB model and some ongoing work for my Doctoral Thesis in this field.
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