Changeset 6260 for trunk/MagicSoft/GRB-Proposal

Timestamp:

02/04/05 16:12:30 (20 years ago)

Author:

gaug

Message:

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File:

• trunk/MagicSoft/GRB-Proposal/Timing.tex (modified) (3 diffs)

trunk/MagicSoft/GRB-Proposal/Timing.tex

@@ -1 +1 @@
 \section{Timing considerations}
 
-The first hint for delayed HE $\gamma$-ray emission from GRBs came with the detection of GRB940217 by the EGRET instrument on board of the Compton Gamma Ray Observatory (CGRO). It was a 18\,GeV photon detected 90\,min. after the burst onset~\cite{EGRET}.
+The first hint for delayed HE $\gamma$-ray emission from GRBs came from the detection by the EGRET detector on board of the Compton Gamma Ray Observatory (CGRO) of 
+a 18\,GeV photon 90\,min. after the onset of 
+GRB940217 by the EGRET detector on board of the Compton Gamma Ray Observatory (CGRO)~\cite{EGRET}.
 
 \par
 
-There are different models that predict prompt and delayed HE $\gamma$-ray emission.
-Most of the models predict HE photons parallel to the keV-MeV burst but also delayed emission is possible. Our main goal should be observation the GRB location as quickly as possible, this is the reason why the \ma telescope is build to slew fast. However, in order to confirm, or rule out different predictions, we should observe the position for a longer period. Our time estimates are based on the following models:
+Different models predict prompt and delayed HE $\gamma$-ray emission.
+Most of them predict HE photons parallel to the keV-MeV burst, 
+but also delayed emission is possible. 
+Our main goal should be to observe the GRB location as quickly as possible. 
+However, in order to confirm or rule out different predictions, 
+we should observe the position for a longer period of time. \\
+
+Our time estimates are based on the following models:
 
 \begin{itemize}
 
-\item Taking into account the fireball model~\cite{REES1,REES2} there are two efficient mechanisms for the generation of VHE photons~\cite{DERISHEV} in GRBs. (1) The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak. This emission should have their highest luminosity together with the main GRB peak. (2) VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks are strongly absorbed by infrared background radiation and cannot be observed from source at cosmological distances. With the presence of an dense ambient medium close to the GRB, the UHE photons will be reprocessed into a softer spectral range. This would lead to VHE emission delayed by few minutes to hours with respect to the beginning of GRB. The timeline including both prozesses is illustrated in figure~\ref{fig:timeline}.
+\item Regarding the fireball model~\cite{REES1,REES2},
+two efficient mechanisms are available for the generation of VHE photons~\cite{DERISHEV}. 
+(1) The prompt emission of $\sim$100\,GeV photons is expected before and during the keV-MeV peak. 
+This emission should have their highest luminosity together with the main GRB peak. 
+(2) VHE photons generated due to inverse Compton (IC) scattering in relativistic shocks 
+are strongly absorbed by infrared background radiation and 
+cannot be observed from cosmological distances. 
+With the presence of a dense ambient medium close to the GRB, 
+the UHE photons will be reprocessed into a softer spectral range. 
+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}.
 
-\item In~\cite{DERMER} two peaks in the GeV light curve are calculated. The first is coincident with the keV-MeV peak, some seconds after the burst onset. The second maximum is peaking at between $\approx$ 1.5 hours up to $\approx$ 25 hours after the burst onset.
+\item In~\cite{DERMER}, two peaks in the GeV light curve are calculated. 
+The first is coincident with the keV-MeV peak, some seconds after the burst onset. 
+The second maximum peaks between $\approx$ 1.5 hours up to $\approx$ 25 hours after the burst onset.
 
-\item Models in~\cite{LI, WANG} 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 after the burst onset. This radiation is accompanied by long-term neutrino emission.
+\item Models in~\cite{LI, WANG} 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 after the onset of the burst. 
+This radiation is accompanied by long-term neutrino emission.
 
 \end{itemize}
@@ -35 +58 @@
 B_{min} \sim \frac{5\times10^{-2}}{\Gamma^{3}}\,
              \frac{\epsilon_{2ph}}{1TeV}\,
-             \frac{t_{GRB}}{10s}\, G
+             \frac{t_{GRB}}{10s}\, G
 \label{eq:minimal}
 \end{equation}
@@ -55 +78 @@
 \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.
+
+%%% Local Variables: 
+%%% mode: latex
+%%% TeX-master: "GRB_proposal_2005"
+%%% End: