The synchrotron-self-Compton radiation accompanying shallow decaying X-ray afterglow: the case of GRB 940217

Abstract

High energy emission (> tens MeV) of Gamma-Ray Bursts (GRBs) provides an important clue to understand the physical processes involved in GRBs, which may be correlated with the GRB early afterglow. A shallow decline phase has been well detected in about half {\it Swift} Gamma-ray Burst X-ray afterglows. The widely considered interpretation involves a significant energy injection and possibly time-evolving shock parameter(s). This work we calculate the synchrotron-self-Compton (SSC) radiation of such an external forward shock and show that it could explain the well-known long term high energy (i.e., tens MeV to GeV) afterglow of GRB 940217. We propose that the cooperation of Swift and GLAST will help to reveal the nature of GRBs.

11 pages, including 1 figure and 1 table

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• A Comprehensive Analysis of Fermi Gamma-Ray Burst Data. I. Spectral Components and Their Possible Physical Origins of LAT/GBM GRBs
• High Energy Afterglow from Gamma-ray Bursts
• High energy gamma-ray emission from Gamma-Ray Bursts -- before GLAST
• Possible Effects of Pair Echoes on Gamma-Ray Burst Afterglow Emission
• Observational Signatures of High-Energy Emission during the Shallow Decay Phase of GRB X-Ray Afterglows
• High energy afterglows and flares from Gamma-Ray Burst by Inverse Compton emission
• MAGIC upper limits on the GRB 090102 afterglow
• GLAST Prospects for Swift-Era Afterglows
• Very High Energy Gamma-ray Afterglow Emission of Nearby Gamma-ray Bursts
• Origin for the Prompt Spectral Evolution Characteristics and High Energy Emission during the X-Ray Flare in GRB 180720B