TITLE:   GCN CIRCULAR
NUMBER:  32780
SUBJECT: GRB 221009A: A type I BdHN of exceptional energetics
DATE:    22/10/17 11:16:22 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.
Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:


GRB221009A detected by Swift (Kennea et al. 2022 GCN32635), Fermi-GBM
(Veres et al. 2022, GCN32636, Lesage et al. 2022, GCN32642), Fermi-LAT
(Bissaldi et al. 2022, GCN32637), with redshift of z=0.151 and an isotropic
equivalent energy of Eiso=2x10^54 erg (de Ugarte Postigo et al. 2022,
GCN32648 and GCN32642) is a typical Binary driven Hypernova of type I
(BdHNI), originating from the collapse of a carbon-oxygen core (CO-core) in
presence of a companion neutron star (NS) with common feature with three
BdHNeI: GRB130427A with "pile up" in the prompt phase (Ruffini et al. 2013,
GCN14526); GRB190114C (Ruffini et al. 2019, GCN23715); and GRB180720B
(Ruffini et al. 2018, GCN23019). As the above three sources, GRB221009A
presents: 1) the optical (Lipunov et al. 2022, GCN32634 and GCN32639;
Perley. 2022 GCN32638; Broens. 2022, GCN32640; Hu et al. 2022, GCN32644;
Mondy: Belkin et al. 2022, GCN32645; de Wet et al.2022, GCN32646; Xu et al.
2022 GCN32647; Odeh 2022, GCN32649; Brivio et al. 2022, GCN32652; Izzo et
al. 2022, GCN32765), radio (Bright et al. 2022, GCN32653 and Farah et al.
2022, GCN32655) and X-ray (Kennea et al, 2022, GCN32635, and GCN32651)
synchrotron afterglow emissions as well as the TeV emission (Yong Huang et
al. 2022, GCN32677), which in BdHNI originate from accreting millisecond
spinning newborn NS (Rueda et al. 2022, e-Print: 2204.00579 [astro-ph.HE]);
2) the ultra-relativistic prompt emission (UPE) phase (Moradi et al. 2021,
PRD 104, 063043 and Rastegarnia et al. 2022, EPJC 82, 778) and GeV emission
(Rueda et al 2022 ApJ 929 56) originated from the black hole formed by
hypercritical accretion of the supernova ejecta on the NS companion; and 3)
the optical emission of the nickel decay of the supernova (SN), created by
the collapse of the CO-core. The first evidence of the supernova rise is
reported by S. Belkin et al. 2022, (GCN32769). In this GRB the bolometric
optical peak of SN is expected to be observed at 15.57+/-2.0 days after the
Fermi-GBM trigger (October 24th 2022, uncertainty from October 22nd 2022 to
October 26th 2022, with the bolometric optical luminosity of
L=(9.45+/-2.8)x10^42 erg/s; Aimuratov et al. in preparation).