Inferring the emission regions for different kinds of gamma-ray bursts

DOI10.1002/ASNA.200610666zbMATH Open1109.85308arXivastro-ph/0608570OpenAlexW3099747440MaRDI QIDQ3424525

Author name not available (Why is that?)

Publication date: 2 March 2007

Published in: Astronomische Nachrichten: A Journal on all Fields of Astronomy (Search for Journal in Brave)

Abstract: Using a theoretical model describing pulse shapes, we have clarified the relations between the observed pulses and their corresponding timescales, such as the angular spreading time, the dynamic time as well as the cooling time. We find that the angular spreading timescale caused by curvature effect of fireball surface only contributes to the falling part of the observed pulses, while the dynamic one in the co-moving frame of the shell merely contributes to the rising portion of pulses provided the radiative time is negligible. In addition, the pulses resulted from the pure radiative cooling time of relativistic electrons exhibit properties of fast rise and slow decay (a quasi-FRED) profile together with smooth peaks. Besides, we interpret the phenomena of wider pules tending to be more asymmetric to be a consequence of the difference in emission regions. Meanwhile, we find the intrinsic emission time is decided by the ratios of lorentz factors and radii of the shells between short and long bursts. Based on the analysis of asymmetry, our results suggest that the long GRB pulses may occur in the regions with larger radius, while the short bursts could locate at the smaller distance from central engine.

Full work available at URL: https://arxiv.org/abs/astro-ph/0608570

zbMATH Keywords

burstsnumerical methodsgamma-rays

Mathematics Subject Classification ID

Hydrodynamic and hydromagnetic problems in astronomy and astrophysics (85A30) Radiative transfer in astronomy and astrophysics (85A25)

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