On GRB 080916C and GRB 090902B observed by the Fermi satellite

Abstract

We propose a possible explanation, in the context of the Fireshell scenario, for the high-energy emission observed in GRB 080916C and GRB 090902B. The physical process underlying this emission consists mainly in the interaction of the baryon in the Fireshell with some high-density region around the burst site. Moreover we associate the observed delay of the onset of the high-energy emission as due to the P-GRB emission

GRB 171010A/SN 2017htp: a GRB-SN at z = 0.33

“…We estimated the star-formation rate and metallicity of the GRB region with different line indicators. The observed properties of the GRB star-forming region (SFR GRB ∼ 0.2 M yr −1 ; 12 + log(O/H) ∼ 8.15 ± 0.10) are similar to those of the star-forming regions hosting other GRBs with an associated Type Ic-BL SN and with available spatially resolved observations (Christensen et al 2008;Krühler et al 2017;Izzo et al 2017;Japelj et al 2018). Long GRBs progenitorstar models and host galaxy observations indicate that long GRBs avoid high-metallicity environments (Vergani et al 2015;Japelj et al 2016;Perley et al 2016;Palmerio et al 2019).…”

“…At 19:00:50.6 UT (=T 0 hereafter) on 2017, October 10, GRB 171010A was detected with the Fermi-LAT and Fermi-GBM instruments (Omodei et al 2017;Poolakkil & Meegan 2017). A few hours later a counterpart was identified near a faint galaxy both in the NIR/optical (Thorstensen & Halpern 2017;Izzo & Malesani 2017) and in the X-rays (D'Aí et al 2017) at coordinates RA = 04:26:19.46, Dec = −10:27:45.9 (J2000).…”