Nearby Sn-Associated Grb 190829a: Environment, Jet Structure, And Vhe Gamma-Ray Afterglows

We present a self-consistent paradigm to interpret the striking features of nearby low-luminosity GRB 190829A. Its prompt gamma-ray lightcurve has two separated pulses. We propose that the interaction of the hard prompt gamma-ray photons (E-p = 624(-303)(+2432) keV) of its initial pulse with the dusty medium (A(V) = 2.33) not only results in the second soft gamma-ray pulse (E-p similar to 12 keV) but also makes a pre-accelerated e(+/-)-rich medium shell via the gamma gamma annihilation. In this paradigm, we show that the observed radio, optical, and X-ray afterglow lightcurves are well-fitted with the forward shock model. Its jet is almost isotropic (theta(j) > 1.0 rad) with a Lorentz factor of similar to 35, and the electron density of the e +/--rich medium shell is similar to 15 cm(-3), which is about seven times higher than the electron density of its normal surrounding medium. The GRB ejecta catches up with and propagates into the e(+/-)-rich medium shell at a region of R = (4.07-6.46) x 10(16) cm. This results in a bright afterglow bump at similar to 10(3) seconds after the GRB trigger. The predicted very high energy (VHE) gamma-ray emission from the synchrotron self-Compton process agrees with the H.E.S.S. observation. The derived broadband spectral energy distribution shows that GRB 190829A like nearby GRBs would be promising targets of the VHE gamma-ray telescopes, such as H.E. S.S., MAGIC, and CTA (Cerenkov Telescope Arrays).