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Title: Search for a Signature of Interaction between Relativistic Jet and Progenitor in Gamma-Ray Bursts

Abstract

The time variability of prompt emission in gamma-ray bursts (GRBs) is expected to originate from the temporal behavior of the central engine activity and the jet propagation in the massive stellar envelope. Using a pulse search algorithm for bright GRBs, we investigate the time variability of gamma-ray light curves to search a signature of the interaction between the jet and the inner structure of the progenitor. Since this signature might appear in the earlier phase of prompt emission, we divide the light curves into the initial phase and the late phase by referring to the trigger time and the burst duration of each GRB. We also adopt this algorithm for GRBs associated with supernovae/hypernovae that certainly are accompanied by massive stars. However, there is no difference between each pulse interval distribution described by a lognorma distribution in the two phases. We confirm that this result can be explained by the photospheric emission model if the energy injection of the central engine is not steady or completely periodic but episodic and described by the lognormal distribution with a mean of ∼1 s.

Authors:
; ;  [1]; ; ;  [2]
  1. College of Science and Engineering, School of Mathematics and Physics, Kanazawa University, Kakuma, Kanazawa, Ishikawa 920-1192 (Japan)
  2. Astrophysical Big Ban Laboratory, RIKEN, Saitama 351-0198 (Japan)
Publication Date:
OSTI Identifier:
22679704
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 849; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALGORITHMS; COSMIC GAMMA BURSTS; DISTRIBUTION; EMISSION; GAMMA RADIATION; INJECTION; INTERACTIONS; PERIODICITY; RELATIVISTIC RANGE; SUPERNOVAE; VISIBLE RADIATION

Citation Formats

Yoshida, Kazuki, Yoneoku, Daisuke, Sawano, Tatsuya, Ito, Hirotaka, Matsumoto, Jin, and Nagataki, Shigehiro, E-mail: yoshida@astro.s.kanazawa-u.ac.jp, E-mail: yonetoku@astro.s.kanazawa-u.ac.jp. Search for a Signature of Interaction between Relativistic Jet and Progenitor in Gamma-Ray Bursts. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA8E48.
Yoshida, Kazuki, Yoneoku, Daisuke, Sawano, Tatsuya, Ito, Hirotaka, Matsumoto, Jin, & Nagataki, Shigehiro, E-mail: yoshida@astro.s.kanazawa-u.ac.jp, E-mail: yonetoku@astro.s.kanazawa-u.ac.jp. Search for a Signature of Interaction between Relativistic Jet and Progenitor in Gamma-Ray Bursts. United States. doi:10.3847/1538-4357/AA8E48.
Yoshida, Kazuki, Yoneoku, Daisuke, Sawano, Tatsuya, Ito, Hirotaka, Matsumoto, Jin, and Nagataki, Shigehiro, E-mail: yoshida@astro.s.kanazawa-u.ac.jp, E-mail: yonetoku@astro.s.kanazawa-u.ac.jp. Wed . "Search for a Signature of Interaction between Relativistic Jet and Progenitor in Gamma-Ray Bursts". United States. doi:10.3847/1538-4357/AA8E48.
@article{osti_22679704,
title = {Search for a Signature of Interaction between Relativistic Jet and Progenitor in Gamma-Ray Bursts},
author = {Yoshida, Kazuki and Yoneoku, Daisuke and Sawano, Tatsuya and Ito, Hirotaka and Matsumoto, Jin and Nagataki, Shigehiro, E-mail: yoshida@astro.s.kanazawa-u.ac.jp, E-mail: yonetoku@astro.s.kanazawa-u.ac.jp},
abstractNote = {The time variability of prompt emission in gamma-ray bursts (GRBs) is expected to originate from the temporal behavior of the central engine activity and the jet propagation in the massive stellar envelope. Using a pulse search algorithm for bright GRBs, we investigate the time variability of gamma-ray light curves to search a signature of the interaction between the jet and the inner structure of the progenitor. Since this signature might appear in the earlier phase of prompt emission, we divide the light curves into the initial phase and the late phase by referring to the trigger time and the burst duration of each GRB. We also adopt this algorithm for GRBs associated with supernovae/hypernovae that certainly are accompanied by massive stars. However, there is no difference between each pulse interval distribution described by a lognorma distribution in the two phases. We confirm that this result can be explained by the photospheric emission model if the energy injection of the central engine is not steady or completely periodic but episodic and described by the lognormal distribution with a mean of ∼1 s.},
doi = {10.3847/1538-4357/AA8E48},
journal = {Astrophysical Journal},
number = 1,
volume = 849,
place = {United States},
year = {Wed Nov 01 00:00:00 EDT 2017},
month = {Wed Nov 01 00:00:00 EDT 2017}
}