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The energetic afterglow of the γ-ray burst of 14 December 1997

机译：1997年12月14日γ射线爆发的高能量余辉

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The discovery of fading but relatively long-lived X-ray emission accompanying γ-ray bursts has revolutionized the study of these objects. This 'afterglow' is most easily explained by models similar to those describing supernovae, but with relativistic ejecta. And as with supernovae, afterglow measurements should in principle provide important constraints on burst properties, permitting, for example, estimates of the amount of energy released, the geometry of the emitting surface and the density of the ambient medium. Here we report infrared observations of the fading optical transient associated with the burst of 14 December 1997 (GRB971214; ref. 6). We detect a 'break' in the broad-band spectrum, as predicted by afterglow models, which constrains the total energy in the burst to be > 10~(51) erg. Combining the fluence of optical afterglow with the redshift (z = 3.42; ref. 7), we estimate that the energy released in the afterglow alone was 2 X 10~(51) erg. Estimates of afterglow energetics are less likely to be subject to geometric effects—such as beaming—that render uncertain estimates of the total burst energy, but it nevertheless appears from our measurements that γ-ray bursts may be much more energetic than the 10~(51) erg usually assumed.
机译：伴随着γ射线爆发而逐渐消失但寿命相对较长的X射线发射的发现，彻底改变了对这些物体的研究。这种“余辉”最容易用类似于描述超新星的模型来解释，但具有相对论性喷射。与超新星一样，余辉测量原则上应对爆发特性提供重要限制，例如，可以估算释放的能量，发射表面的几何形状和周围介质的密度。在这里，我们报告了与1997年12月14日爆发有关的衰落光学瞬变的红外观测结果（GRB971214；参考文献6）。正如余辉模型所预测的，我们在宽带频谱中检测到“断裂”，从而将猝发中的总能量限制为> 10〜（51）erg。结合光学余辉与红移的能量密度（z = 3.42；参考文献7），我们估计仅余辉释放的能量为2 X 10〜（51）erg。余辉能量的估计不太可能受到几何效应的影响，例如射束，从而无法确定总爆发能量的估计，但是从我们的测量结果来看，γ射线爆发的能量可能比10〜（）高得多。 51）通常假定。

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