Evidence for a Canonical Gamma‐Ray Burst Afterglow Light Curve in the<i>Swift</i>XRT Data

TLDR

We present new observations of the early X‑ray afterglows of the first 27 GRBs observed with Swift XRT. The Swift XRT provided well‑sampled early afterglow light curves for these GRBs. The light curves exhibit a canonical three‑segment power‑law decay (steep, shallow, then steeper) with breaks at ≲500 s and 10³–10⁴ s, often punctuated by X‑ray flares from late central‑engine activity, and the steep decay is attributed to the prompt‑emission tail while the shallow phase reflects continuous energy injection that boosts the afterglow shock energy by at least a factor of four.

Abstract

We present new observations of the early X-ray afterglows of the first 27 gamma-ray bursts (GRBs) well observed by the Swift X-Ray Telescope (XRT). The early X-ray afterglows show a canonical behavior, where the light curve broadly consists of three distinct power-law segments: (1) an initial very steep decay (∝t-α with 3 ≲ α1 ≲ 5), followed by (2) a very shallow decay (0.5 ≲ α2 ≲ 1.0), and finally (3) a somewhat steeper decay (1 ≲ α3 ≲ 1.5). These power-law segments are separated by two corresponding break times, tbreak,1 ≲ 500 s and 103 s ≲ tbreak,2 ≲ 104 s. On top of this canonical behavior, many events have superimposed X-ray flares, which are most likely caused by internal shocks due to long-lasting sporadic activity of the central engine, up to several hours after the GRB. We find that the initial steep decay is consistent with it being the tail of the prompt emission, from photons that are radiated at large angles relative to our line of sight. The first break in the light curve (tbreak,1) takes place when the forward shock emission becomes dominant, with the intermediate shallow flux decay (α2) likely caused by the continuous energy injection into the external shock. When this energy injection stops, a second break is then observed in the light curve (tbreak,2). This energy injection increases the energy of the afterglow shock by at least a factor of f ≳ 4 and augments the already severe requirements for the efficiency of the prompt gamma-ray emission.