TY - JOUR
T1 - High-energy emission as a test of the prior emission model for gamma-ray burst afterglows
AU - Murase, Kohta
AU - Toma, Kenji
AU - Yamazaki, Ryo
AU - Nagataki, Shigehiro
AU - Ioka, Kunihito
PY - 2010/2
Y1 - 2010/2
N2 - We study high-energy gamma-ray afterglow emission from gamma-ray bursts (GRBs) in the prior emission model, which is proposed to explain the plateau phase of the X-ray afterglow. This model predicts the high-energy gamma-ray emission when the prompt GRB photons from the main flow are up-scattered by relativistic electrons accelerated at the external shock due to the prior flow. The expected spectrum has the peak of ~10-100 GeV at around the end time of the plateau phase for typical GRBs, and high-energy gamma-rays from nearby and/or energetic GRBs can be detected by the current and future Cherenkov telescopes such as MAGIC, VERITAS, CTA and possibly Fermi. Multiwavelength observations by ground-based optical telescopes as well as Fermi and/or Swift satellites are important to constrain the model. Such external inverse-Compton emission may even lead to GeV-TeV gamma-ray signals with the delay time of ~10-100 s, only if the plateau phase is short lived.
AB - We study high-energy gamma-ray afterglow emission from gamma-ray bursts (GRBs) in the prior emission model, which is proposed to explain the plateau phase of the X-ray afterglow. This model predicts the high-energy gamma-ray emission when the prompt GRB photons from the main flow are up-scattered by relativistic electrons accelerated at the external shock due to the prior flow. The expected spectrum has the peak of ~10-100 GeV at around the end time of the plateau phase for typical GRBs, and high-energy gamma-rays from nearby and/or energetic GRBs can be detected by the current and future Cherenkov telescopes such as MAGIC, VERITAS, CTA and possibly Fermi. Multiwavelength observations by ground-based optical telescopes as well as Fermi and/or Swift satellites are important to constrain the model. Such external inverse-Compton emission may even lead to GeV-TeV gamma-ray signals with the delay time of ~10-100 s, only if the plateau phase is short lived.
KW - Gamma rays: bursts
KW - Gamma-rays: theory
KW - Radiation mechanisms: non-thermal
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U2 - 10.1111/j.1745-3933.2009.00799.x
DO - 10.1111/j.1745-3933.2009.00799.x
M3 - Letter
AN - SCOPUS:79251528973
SN - 1745-3925
VL - 402
SP - L54-L58
JO - Monthly Notices of the Royal Astronomical Society: Letters
JF - Monthly Notices of the Royal Astronomical Society: Letters
IS - 1
ER -