(GRB ) 一条 gamma 光线的轴什么时候爆炸了，不与它的来源的旋转轴与一致，可以在那里结果一口圆形的喷气。用一些精制喷气动力学，我们计算晚霞光为如此的圆形的喷气弄弯的多波长。被许多参数在我们由于微笑的效果和裂缝在晚霞光曲线发现一个明显的裂缝的R乐队影响，例如电子精力部分ξ
e ,磁性的精力部分ξ
B 2,戒指Δθ和中等数字密度 n 的宽度。全面轻曲线能被划分成三个幂定律舞台，即，一个极端相对论的舞台，一个在打破以后舞台和一个深牛顿的舞台。为每个舞台，幂定律索引比在相应圆锥形的喷气在圆形的喷气是更大的。
Extensive multi-band afterglow data are available for GRB 980703. Especially,its radio afterglow was very bright and was monitored until more than 1000 days after the trigger time. Additionally,there is no obvious special feature,i.e.,no rebrightenings,no plateau,and no special steep decay or slow decay in the multi-band afterglow light curves. All these conditions make GRB 980703 a precious sample in gammaray burst research. Here we use the observational data of GRB 980703 to test the standard fireball model in depth. It is found that the model can give a satisfactory explanation to the multi-band and overall afterglow light curves. The beaming angle of GRB 980703 is derived as ～ 0.23 radian,and the circum-burst medium density is ～ 27 cm-3. The total isotropic equivalent kinetic energy of the ejecta is ～ 3.8 × 1052 ergs. A rest-frame extinction of AV ～ 2.5 mag in the host galaxy is also derived.
Multiple rebrightenings have been observed in the multiband afterglow of GRB 030329.In particular,a marked and quick rebrightening occurred at about t ～ 1.2 × 105 s.Energy injection from late and slow shells seems to be the best interpretation for these rebrightenings.Usually it is assumed that the energy is injected into the whole external shock.However,in the case of GRB 030329,the rebrightenings are so quick that the usual consideration fails to give a satisfactory fit to the observed light curves.Actually,since these late/slow shells freely coast in the wake of the external shock,they should be cold and may not expand laterally.The energy injection then should only occur at the central region of the external shock.Considering this effect,we numerically re-fit the quick rebrightenings observed in GRB 030329.By doing this,we were able to derive the beaming angle of the energy injection process.Our result,with a relative residual of only 5%-10% during the major rebrightening,is better than any previous modeling.The derived energy injection angle is about 0.035.We assume that these late shells are ejected by the central engine via the same mechanism as those early shells that produce the prompt gamma-ray burst.The main difference is that their velocities are much slower,so that they catch up with the external shock relatively late and are manifested as the observed quick rebrightenings.If this were true,then the derived energy injection angle can give a good measure of the beaming angle of the prompt γ-ray emission.Our study may hopefully provide a novel method to measure the beaming angle of gamma-ray bursts.
A long plateau phase and an amazing level of brightness have been observed in the X-ray afterglow of GRB 060729.This peculiar light curve is likely due to longterm energy injection in external shock.Here,we present a detailed numerical study of the energy injection process of magnetic dipole radiation from a strongly magnetized millisecond pulsar and model the multi-band afterglow observations.It is found that this model can successfully explain the long plateaus in the observed X-ray and optical afterglow light curves.The sharp break following the plateaus could be due to the rapid decline of the emission power of the central pulsar.At an even later time(～5×106 s) ,an obvious jet break appears,which implies a relatively large half opening angle of θ～ 0.3 for the GRB ejecta.Due to the energy injection,the Lorentz factor of the outflow is still larger than two even at 107 s after the GRB trigger,making the X-ray afterglow of this burst detectable by Chandra even 642d after the burst.
