Index: /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6162) +++ /trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex (revision 6163) @@ -59,5 +59,5 @@ M. Garczarczyk\\ \texttt{}\\ M. Gaug\\ \texttt{} \\ - S. Mizobuchi\\ \texttt{} + S. Mizobuchi\\ \texttt{} } @@ -167,4 +167,9 @@ \bibitem{ecl} Private communication with Lorenz E. + +%References used in Timing +\bibitem{DERISHEV} Derishev E.V., Kocharovsky V.V., Kocharovsky VI.V., +AIP Conf.Proc.558:405-416,2001 + %Not used references Index: /trunk/MagicSoft/GRB-Proposal/Introduction.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6162) +++ /trunk/MagicSoft/GRB-Proposal/Introduction.tex (revision 6163) @@ -75,8 +75,18 @@ -\subsection{Observation of Soft Gamma Repeaters(SGRs)} -A stronge magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' p -eriodically emit gamma-ray, and are extremely rare stars. Only four identified -SGRs are discovered in the last 20 years: SGR0526-66, SGR1806-20, SGR1900+14, SG -R1627-41. GRBs and SGRs can be explained with an unique precessing gamma jet mod -el observed at different beam-angle and at different ages. +\subsection{Observation of SGRs} +A stronger magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' periodically emit gamma-ray, and are extremely rare stars. Only four identified +SGRs are discovered in the last 20 years: SGR0526-66, SGR1806-20, SGR1900+14, SGR1627-41. GRBs and SGRs can be explained with an unique processing gamma jet model observed at different beam-angle and at different ages.\\ +\par +The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30 Jan 05. The fluence is $\sim$ 1$\times$10$^{-5}$erg/cm$^2$(15-350keV). This event have five orders of magnitude smaller than the giant flare from this source on 27 Dec 04. If a giant flare from SGR occurs as SGR1806-20, MAGIC has enough sensitivity for 100 second observation time.\\ +\par +MAGIC and Gamma-ray satellites react in the same way for also SGRs. + + + + + + + + + Index: /trunk/MagicSoft/GRB-Proposal/Timing.tex =================================================================== --- /trunk/MagicSoft/GRB-Proposal/Timing.tex (revision 6162) +++ /trunk/MagicSoft/GRB-Proposal/Timing.tex (revision 6163) @@ -1,20 +1,33 @@ \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.} +The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\ + +%\subsection{Determine reasonable upper limit for observation duration } +According to the some calculation~\cite{DERISHEV}, GRB produces VHE emission consisting of three components, which have different spectral and time profile. Prompt emission of $\sim$ 100GeV photons should be observed prior to or during the GRB main pulse. During the GRB main pulse, the highest luminosity should be observed. The reprocessed photons from 10\% of GRB can be observed by ground-based experiments with sub-TeV energy range. Third component lasts longer than the GRB main pulse. The duration time of this component is from minutes to hours.\\ \par +For reprocessing of VHE Photons, the definition of minimal value B$_min$ is following. +\begin{equation} +B_{min} \sim \frac{5\times10^{-2}}{\Gamma^{3}}\, + \frac{\epsilon_{2ph}}{1TeV}\, + \frac{t_{GRB}}{10s}\, G +\label{eq:minimal} +\end{equation} +And the duration time of delay of reprocessed VHE emission may by calculated via the following function: +\begin{equation} +t_{d} \simeq \frac{2^{4/3}}{3} \biggl(\frac{B_{\perp}}{B_{min}}\biggl)^{2/3} +\label{eq:duration} +\end{equation} +When absorption threshold$\epsilon_{2ph}$ is 1TeV, duration time of GRB main pulse is 10$^{2}$s, Lorentz factor of the GRB shell $\Gamma$ is 10$^{2}$, the duration of delayed VHE emission is about 0.8 hours for component of magnetic field perpendicular to electron's trajectory B$_{\perp}$ of 0.1 [Gauss], 3.6 hours for 1.0 [Gauss] and 17.3 hours for 10 [Gauss].\\ +\par +In~\cite{DERMER}, two peaks in the GeV light curve are calculated. An early maximum coincident with the MeV peak is some seconds after the burst onset. The second maximum peaking at $\approx$ 1.5 hours is up to 10$^5$ sec. ($\approx$ 25 hours) after the burst.\\ +\par +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).\\ +\par +It is not so easy to say a reasonable observation time after GRBs, because GRB has its own characteristic and time profile. But, if it is possible to point to the GRB sources before finishing a GRB main pulse and continue to observe for 5 hours, we can put some constraints on parameters of GRB sources. -The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\ -\par -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.\\ -\par -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). -\par -\ldots \textit{\bf UNTIL WHEN WILL WE OBSERVE THE BURST AFTER OCCURRANCE} \ldots -\par -\subsection{Determine reasonable upper limit for observation duration } + +