source: trunk/MagicSoft/GRB-Proposal/Timing.tex@ 6158

\section{Timing considerations}

{\it Here, all possible models should go in with reasonning why certain time 
or flux estimates are proposed.  We have now only estimates on extrapolations 
of the \eg power-laws. Maybe we should include: IC (in many possible combinations), hadronic emission models (see~\cite{TASC}), Cannonball model.}
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The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\
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In~\cite{DERMER}, two peaks in the GeV light curve are calculated. An early maximum coincident with the MeV peak is the high-energy extension of the synchrotron component, some seconds after the burst onset. The second maximum peaking at $\approx$ 1.5 hours is due primarily to SSC radiation with significant emission of up to $10^5$ sec. ($\approx 25$ hours) after the burst.\\
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Li, Dai and Lu~\cite{LI} suggest GeV emission after pion production and some thermalization of the UHE component with radiation maxima of up to one day or even one week (accompanied by long-term neutrino emission).

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\ldots \textit{\bf UNTIL WHEN WILL WE OBSERVE THE BURST AFTER OCCURRANCE}   \ldots
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\subsection{Determine reasonable upper limit for observation duration }