On the Non-existence of a Sharp Cooling Break in Gamma-Ray Burst Afterglow Spectra
Authors: Z. Lucas Uhm and Bing Zhang
Uhm & Zhang
2014 The Astrophysical Journal78082.
Provider: AAS Journals
Caption: Figure 5.
Comparison between two different profiles: solid line for spectra from Figure
4 (BM profile) and dotted line for spectra from Figure
1 (constant profile). Left:
B = 0.001 (slow cooling). Right:
B = 0.1 (fast cooling).
B
= 0.001 (slow cooling). Right:
