Inverse compton radiation from GRB afterglows in the VHE range

Jagdish C. Joshi; Soebur Razzaque

Inverse compton radiation from GRB afterglows in the VHE range

Jagdish C. Joshi, Soebur Razzaque

Physics

University of Johannesburg

Research output: Contribution to journal › Conference article › peer-review

Abstract

The observation of Gamma-ray bursts (GRBs) can be classified into prompt and afterglow emission. The prompt emission is observed for up to 100s of seconds after the trigger of the event while a delayed and long-lasting afterglow emission is followed after this phase. The prompt emission dominates in the γ-rays (keV-MeV-GeV), while the afterglow emission mainly occurs in X-ray, UV, optical, radio wavelengths and possibly in γ-rays. In this work, we study the signature of inverse Compton emission in the afterglow emission of GRBs. We consider the expansion of an adiabatic blast wave into a constant density medium and use the observation of GRB 130427A afterglow to constrain the model parameters. The flux produced via inverse-Compton mechanism have been discussed and also possible detection by the Cherenkov Telescope Array mainly in the range 30 GeV- 1 TeV have been discussed.

Original language	English
Journal	Proceedings of Science
Volume	338
Publication status	Published - 2018
Event	6th High Energy Astrophysics in Southern Africa, HEASA 2018 - Parys, Free State, South Africa Duration: 1 Aug 2018 → 3 Aug 2018

ASJC Scopus subject areas

Multidisciplinary

Cite this

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title = "Inverse compton radiation from GRB afterglows in the VHE range",

abstract = "The observation of Gamma-ray bursts (GRBs) can be classified into prompt and afterglow emission. The prompt emission is observed for up to 100s of seconds after the trigger of the event while a delayed and long-lasting afterglow emission is followed after this phase. The prompt emission dominates in the γ-rays (keV-MeV-GeV), while the afterglow emission mainly occurs in X-ray, UV, optical, radio wavelengths and possibly in γ-rays. In this work, we study the signature of inverse Compton emission in the afterglow emission of GRBs. We consider the expansion of an adiabatic blast wave into a constant density medium and use the observation of GRB 130427A afterglow to constrain the model parameters. The flux produced via inverse-Compton mechanism have been discussed and also possible detection by the Cherenkov Telescope Array mainly in the range 30 GeV- 1 TeV have been discussed.",

author = "Joshi, {Jagdish C.} and Soebur Razzaque",

note = "Publisher Copyright: {\textcopyright} Copyright owned by the author(s) under the terms of the Creative Commons.; 6th High Energy Astrophysics in Southern Africa, HEASA 2018 ; Conference date: 01-08-2018 Through 03-08-2018",

year = "2018",

language = "English",

volume = "338",

journal = "Proceedings of Science",

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TY - JOUR

T1 - Inverse compton radiation from GRB afterglows in the VHE range

AU - Joshi, Jagdish C.

AU - Razzaque, Soebur

N1 - Publisher Copyright: © Copyright owned by the author(s) under the terms of the Creative Commons.

PY - 2018

Y1 - 2018

N2 - The observation of Gamma-ray bursts (GRBs) can be classified into prompt and afterglow emission. The prompt emission is observed for up to 100s of seconds after the trigger of the event while a delayed and long-lasting afterglow emission is followed after this phase. The prompt emission dominates in the γ-rays (keV-MeV-GeV), while the afterglow emission mainly occurs in X-ray, UV, optical, radio wavelengths and possibly in γ-rays. In this work, we study the signature of inverse Compton emission in the afterglow emission of GRBs. We consider the expansion of an adiabatic blast wave into a constant density medium and use the observation of GRB 130427A afterglow to constrain the model parameters. The flux produced via inverse-Compton mechanism have been discussed and also possible detection by the Cherenkov Telescope Array mainly in the range 30 GeV- 1 TeV have been discussed.

AB - The observation of Gamma-ray bursts (GRBs) can be classified into prompt and afterglow emission. The prompt emission is observed for up to 100s of seconds after the trigger of the event while a delayed and long-lasting afterglow emission is followed after this phase. The prompt emission dominates in the γ-rays (keV-MeV-GeV), while the afterglow emission mainly occurs in X-ray, UV, optical, radio wavelengths and possibly in γ-rays. In this work, we study the signature of inverse Compton emission in the afterglow emission of GRBs. We consider the expansion of an adiabatic blast wave into a constant density medium and use the observation of GRB 130427A afterglow to constrain the model parameters. The flux produced via inverse-Compton mechanism have been discussed and also possible detection by the Cherenkov Telescope Array mainly in the range 30 GeV- 1 TeV have been discussed.

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M3 - Conference article

AN - SCOPUS:85070917833

SN - 1824-8039

VL - 338

JO - Proceedings of Science

JF - Proceedings of Science

T2 - 6th High Energy Astrophysics in Southern Africa, HEASA 2018

Y2 - 1 August 2018 through 3 August 2018

ER -

Inverse compton radiation from GRB afterglows in the VHE range

Abstract

ASJC Scopus subject areas

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