GCN Circular 32808
Subject
GRB 221009A: Peak luminosity of the supernova vs. synchrotron afterglow
Date
2022-10-20T14:57:47Z (2 years ago)
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:
GRB 221009A appears to be a rare example (Jean-Luc Atteia et al. 2022, GCN
32793) of a particularly energetic and close GRB (de Ugarte Postigo et al.
2022, GCN 32648 and Lesage et al. 2022, GCN 32642 and N.P.M. Kuin et al.
2022, GCN 32656). Within the BdHN model, we have followed the X-ray,
optical, and radio afterglows originating from synchrotron emission powered
by fast spinning newborn neutron stars (vNS) with initial periods of
fraction of a millisecond, accreting the supernova ejecta, created by the
collapse of a carbon-oxygen core (Rueda et al. 2022, arXiv:2204.00579).
Figures 1, 2 and 3 show the afterglows of three type I BdHNe, namely GRB
180720B (Ruffini et al. 2018, GCN 23019), GRB 190114C (Ruffini et al. 2019,
GCN 23715), and GRB 211023A (Aimuratov et al. 2021, GCN 31056), and the
prediction of their associated supernova.
We have indicated the expected time of the occurrence of the supernova in
GRB 221009A (Aimuratov et al. 2022, GCN 32780). The ongoing observations in
optical, radio, and X-ray bands are strongly recommended for allowing the
determination of the spin and magnetic field of the vNS. This will probe as
well if the optical synchrotron emission, at ~ 10^6 s from the Fermi-GBM
trigger, impedes the observations of the optical emission of the supernova
originating from nickel decay (Aimuratov et al. in preparation, see also
data from Ilfan Bikmaev et al. 2022, GCN 32752, and Jia. Ren et al. 2022,
arXiv:2210.10673, reproduced in Fig. 4).
Fig1: http://www.icranet.org/docs/Fig1.pdf
Fig2: http://www.icranet.org/docs/Fig2.pdf
Fig3: http://www.icranet.org/docs/Fig3.pdf
Fig4: http://www.icranet.org/docs/Fig4.pdf