Changeset 6163 for trunk

Timestamp:

02/01/05 03:23:54 (20 years ago)

Author:

satoko

Message:

*** empty log message ***

Location:

trunk/MagicSoft/GRB-Proposal

Files:

• GRB_proposal_2005.tex (modified) (2 diffs)
• Introduction.tex (modified) (1 diff)
• Timing.tex (modified) (1 diff)

trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex

@@ -59 +59 @@
   M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\
   M. Gaug\\ \texttt{<markus@ifae.es>} \\
-  S. Mizobuchi\\ \texttt{<satoko@icrr.u-tokyo.ac.jp>}
+  S. Mizobuchi\\ \texttt{<satoko@mppmu.mpg.de>}
 }
 
@@ -167 +167 @@
 \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
 

trunk/MagicSoft/GRB-Proposal/Introduction.tex

@@ -75 +75 @@
 
 
-\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. 
+
+
+
+
+
+
+
+
+

trunk/MagicSoft/GRB-Proposal/Timing.tex

@@ -1 +1 @@
 \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 }
+
+