Table 1
Properties of four bursts discussed in this study.
| GRB | SB | 080916C | 090902B | 091024 |
|
|
||||
| α γ | 1 | 0.91 | 0.61 | 1.01 |
| β γ | 2 | 2.08 | 3.80 | 2.17 |
| ϵγ,break [MeV] | 1.556 | 0.167 | 0.613 | 0.081 |
| Γ | 102.5 | 1090 | 1000 | 195 |
| tv [s] | 0.0045 | 0.1 | 0.053 | 0.032 |
| T90 [s] | 30 | 66 | 22 | 196 |
| z | 2 | 4.35 | 1.822 | 1.09 |
| Sγ [erg cm-2] | 1 × 10-5 | 1.6 × 10-4 | 3.3 × 10-4 | 5.1 × 10-5 |
| Liso [erg s-1] | 1052 | 4.9 × 1053 | 3.6 × 1053 | 1.7 × 1051 |
Notes. See Baerwald et al. (2011)
for SB (“standard burst”, similar shape to Waxman
& Bahcall 1997, 1999); Nava et al. (2011), Greiner et al. (2009) for GRB 080916C; Nava
et al. (2011), Abdo et al. (2009) for
GRB 090902B and Nava et al. (2011), Gruber et al. (2011) for GRB 091024. The luminosity
is calculated with 
, with
Sγ the fluence in
the (bolometrically adjusted) energy range 1 keV–10 MeV. For the gamma-ray spectrum, a
broken power law is assumed with spectral index αγ below the break,
βγ above the break,
and the break energy ϵγ,break. Adopted
from Hümmer (2013).
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