The bumpy light-curve of the bright optical afterglow (AG) of gamma ray burst (GRB) 021004, its spectral evolution and its radio emission have been claimed to be unusual. In the Cannonball Model of GRBs that is not the case. The very early AG's shape is, as for GRB 990123, a direct tracer of the expected circumburst density profile. The unprecedented… (More)
Fig. 1.— Comparison between the NIR–optical observations of the AG of GRB 021004 and the CB model fit for two CBs with different parameters, each contributing as in Eqs. (1) to (4). The ISM density was assumed to be a constant plus an additional “wind” contribution decreasing as 1/r2. The figure shows (from top to bottom) 104 times the K band, 103 times the H band, 102 times the J band, 10 times the I-band, the R-band, 10−1 of the V-band and 10−2 of the B-band. These data are from: Fox et al. 2002; Matsumoto et al. 2002a,b; Oksanen et al. 2002a,b; Weidinger et al. 2002; Winn et al. 2002; Zharikov et al. 2002; Halpern et al. 2002a,b; Balman et al. 2002; Anupama et al. 2002; Cool et al. 2002; Holland et al. 2002a,b; Bersier et al. 2002; Sahu et al. 2002a,b; Torii et al. 2002; Covino et al. 2002a,b; Stanek et al. 2002; Rhoads et al. 2002; Mirabal et al. 2002a,b; Masetti et al. 2002, Barsukova et al. 2002; Malesani et al. 2002a,b; Klotz et al. 2002a,b; Di Paola et al. 2002; Stefanon et al. 2002: Lindsay et al. 2002a,b; and Williams et al. 2002; all recalibrated with the observations of Henden et al. (2002). The bottom line is the CB model prediction of the synchrotron contribution to the 2-10 keV X-ray AG (Datum is from Sako et al. 2002).