Index: trunk/MagicSoft/GRB-Proposal/Timing.tex
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--- trunk/MagicSoft/GRB-Proposal/Timing.tex	(revision 6260)
+++ trunk/MagicSoft/GRB-Proposal/Timing.tex	(revision 6261)
@@ -29,5 +29,5 @@
 This would lead to VHE emission delayed by few minutes to hours with 
 respect to the beginning of GRB. 
-The timeline including both processes is illustrated in figure~\ref{fig:timeline}.
+The time-line including both processes is illustrated in figure~\ref{fig:timeline}.
 
 \item In~\cite{DERMER}, two peaks in the GeV light curve are calculated. 
@@ -44,14 +44,19 @@
 \centering
 \includegraphics[width=0.6\linewidth]{GRBbrigthness.eps}
-\caption{A possible example of GRB timeline as verified in~\cite{DERISHEV}}
+\caption{A possible example of GRB time-line as depicted in~\cite{DERISHEV}}
 \label{fig:timeline}
 \end{figure}
 
-Based on the model in~\cite{DERISHEV}, three different components of VHE emission exists in an GRB. This components are illustrated in figure~\ref{fig:timeline}. (a) There is the prompt 100\,GeV peak before and during the first keV-MeV peak, (b) the VHE emission due to inverse Compton scattering lasting for the whole duration of the GRB pulse and (c) the reprocessed inverse Compton emission which may last up to hours after the GRB onset.
+Based on the model in~\cite{DERISHEV}, three different components of VHE emission exists in an GRB. 
+The corresponding components are illustrated in figure~\ref{fig:timeline}. 
+(a) There is the prompt 100\,GeV peak before and during the first keV-MeV peak, 
+(b) the VHE emission due to Inverse Compton scattering lasting for the whole duration of the GRB pulse and 
+(c) the reprocessed Inverse Compton emission which may last up to hours after the GRB onset.
 (b) and (c) are the components which may be detectable by \ma and other ground based $\gamma$-ray detectors.
 
 \par
 
-To achive significant emission due to inverse Comton scattering of the sub-MeV radiation, a minimal magnetic field $B_{min}$ is necessary:
+To achieve significant emission due to inverse Compton scattering 
+of the sub-MeV radiation, a minimal magnetic field $B_{min}$ is necessary:
 
 \begin{equation}
@@ -62,5 +67,7 @@
 \end{equation}
 
-When the magnetic field is much stronger than $B_{min}$, the delay of reprocessed photons may become observable. For this perpendicular case it can be calculated via the following asymptotic expression:
+If the magnetic field is much stronger than $B_{min}$, 
+the delay of reprocessed photons may become observable. 
+For this perpendicular case it can be calculated via the following asymptotic expression:
 
 \begin{equation}
@@ -69,13 +76,23 @@
 \end{equation}
 
-For typical values of the absorption threshold $\epsilon_{2ph}=1\,TeV$, duration time of GRB main pulse $t_{GRB}=10^{2}\,s$ and Lorentz factor of the GRB shell $\Gamma=10^{2}$, the duration of delayed VHE emission will be 0.8 hours for the component of magnetic field perpendicular to electron's trajectory $B_{\perp}=0.1\,Gauss$, 3.6 hours for $B_{\perp}=1.0\,Gauss$ and 17.3 hours for $B_{\perp}=10\,Gauss$.\\
+For typical values of the absorption threshold $\epsilon_{2ph}=1\,TeV$, 
+the duration time of GRB main pulse $t_{GRB}=10^{2}\,s$ and Lorentz factor of the GRB shell 
+$\Gamma=10^{2}$, the duration of delayed VHE emission will be 0.8 hours for the component of magnetic 
+field perpendicular to electron's trajectory $B_{\perp}=0.1\,Gauss$, 
+3.6 hours for $B_{\perp}=1.0\,Gauss$ and 17.3 hours for $B_{\perp}=10\,Gauss$.\\
 
-Observation of the delayed VHE emission and the time correlation will give informations about the density of the surrounding interstellar gas, the magnetic field and the Lorentz factor of the GRB shell.\\
+The observation of the delayed VHE emission and the time correlation will give informations 
+about the density of the surrounding interstellar gas, the magnetic field and 
+the Lorentz factor of the GRB shell.\\
 
-It is not easy to fix a reasonable observation time of a GRB based on the described models. Every bust has its own characteristic and time profile. Hovewer, obseration of the GRB coordinates for/within 5 hours after the alert may put constraints on model parameters of GRB sources.\\
+It is not easy to determine a reasonable observation time of a GRB based on the described models. 
+Every burst has its own characteristic and time profile. 
+However, observation of the GRB coordinates for/within 5 hours after the alert may set 
+constraints on model parameters of GRB sources.\\
 
-In case of an \textcolor{red}{\bf Red Alarm}, we propose to take data for {\bf 5 hours}.
+In the case of an \textcolor{red}{\bf Red Alarm}, we propose to take data for {\bf 5 hours}.
 \par
-In case of an \textcolor{yellow}{\bf Yellow Alarm}, we propose to observe the source from the time when it will become observable until the {\bf 5 hours} pass.
+In the case of an \textcolor{yellow}{\bf Yellow Alarm}, 
+we propose to observe the source from the time when it will become observable until the {\bf 5 hours} pass.
 
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