The afterglow phase is well studied unlike the prompt phase. The GRB afterglow observations provide the redshift of the the burst which shed light on the constituents of ISM and the underlying physical processes (Greiner, J. et al. 2009; Gendre, B. & Boër, M. 2005; Schady 2015). The broadband observation of the afterglow phase conveys broad picture of the energetics and timeline of the underlying processes.
During the main prompt GRB phase, the source invoke highly relativistic jets with bulk Lorentz factors of a few hundreds emitting highly energetic photons. The exact physical mechanism producing such powerful γ-rays still remains debated (Kumar & Zhang 2015). The composition of GRB jets, the radiative processes giving rise to the prompt γ-rays are some of the open ended questions (Kumar & Zhang 2015). Both in terms of spectral properties and physical mechanisms, prompt emissions are still comparatively poorly explored (Zhang 2011) as opposed to the afterglow phase due to the transient nature of the event and lack of observations in the soft X-ray band (Gehrels & Mészáros 2012; Oganesyan, G. et al. 2018). Daksha mission is expected to improve over both these aspects with its all-sky capability and ability to probe in soft X-ray band and hence improving the population of the GRBs. Below, we highlight on the GRB science we can probe with the Daksha mission especially in the prompt phase.