Abstract
Gamma-ray bursts (GRBs) are ideal probes of the epoch of the first stars and galaxies. We review the recent theoretical understanding of the formation and evolution of the first (so-called Population III) stars, in light of their viability of providing GRB progenitors. We proceed to discuss possible unique observational signatures of such bursts, based on the current formation scenario of long GRBs. These include signatures related to the prompt emission mechanism, as well as to the afterglow radiation, where the surrounding intergalactic medium might imprint a telltale absorption spectrum. We emphasize important remaining uncertainties in our emerging theoretical framework.
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Notes
It may be misleading to state “devoid of metals”. Pop III GRB progenitors via CHE, for example, could have ejected CNO elements into the surrounding medium via mass shedding during the late stages of their evolution.
Recently, GRBs from supermassive stars with \(M \sim10^{5}~\mathrm{M}_{\odot}\) which could make seed BHs for supermassive BHs are also discussed (Matsumoto et al. 2015).
Mizuta and Ioka (2013) propose an alternative scenario that the duration of the bright part of the prompt emission is determined by an increase of \(\theta_{j}\) on a timescale of the pressure decay of the cocoon emerging from the progenitor star.
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Acknowledgements
K.T. thank P. Mészáros, K. Ioka, Y. Suwa, and D. Nakauchi for useful comments. This work is partly supported by JSPS Grants-in-Aid for Scientific Research 15H05437 (K.T.), JST grant “Building of Consortia for the Development of Human Resources in Science and Technology” (K.T.) and NSF grant AST-1211729 (V.B.). SCY was supported by Basic Science Research (2013R1A1A2061842) program through the National Research Foundation of Korea (NRF).
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Toma, K., Yoon, SC. & Bromm, V. Gamma-Ray Bursts and Population III Stars. Space Sci Rev 202, 159–180 (2016). https://doi.org/10.1007/s11214-016-0250-7
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DOI: https://doi.org/10.1007/s11214-016-0250-7