Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..142..443t&link_type=abstract
Astronomy and Astrophysics Supplement, v.142, p.443-445
Astronomy and Astrophysics
Astrophysics
2
Gamma-Ray Bursts (Grb)
Scientific paper
Some recent experiments detecting very high energy (VHE) gamma-rays above 10-20 TeV, independently reported VHE bursts for some bright gamma-ray bursts (GRBs), although further confirmation is necessary. If these signals are truly from GRBs, these GRBs must emit a much larger amount of energy as VHE gamma-rays than in the ordinary photon energy range of GRBs (keV-MeV). We show that such extreme phenomena can be reasonably explained by synchrotron radiation of protons accelerated to ~ 1020-21 eV. Protons must carry a much larger amount of energy than electrons, suggesting that energy transfer from protons into electrons in shocked matter is very inefficient. The total energy of GRBs becomes as large as gtilde 1055 (Delta Omega / 4 pi ) ergs and hence a strong beaming of GRB emission is highly likely. There may also be TeV emission in afterglow phase from external shocks, and proton synchrotron in this phase gives a quantitative explanation for the famous long duration GeV emission from GRB 940217. Most TeV gamma-rays are absorbed in intergalactic space by interactions with the infrared and microwave background radiations, and finally form gamma-ray background in GeV range. This process may explain the extragalactic background radiation observed in the EGRET range. We also discuss absorption of TeV gamma-rays in the shocked region of GRBs by the gamma gamma -> e\pm process, which may provide a new channel for energy transfer from protons into electrons (and positrons). This process should be important for the energetics of GRBs. This article had been submitted as a contribution paper in the ``Rome '98 Gamma-Ray Burst workshop'' and should have appeared in the A\&AS special issue for the workshop (A\&AS 1999, 138 (3)).
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