Changeset 6163 for trunk/MagicSoft


Ignore:
Timestamp:
02/01/05 03:23:54 (20 years ago)
Author:
satoko
Message:
*** empty log message ***
Location:
trunk/MagicSoft/GRB-Proposal
Files:
3 edited

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  • trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex

    r6162 r6163  
    5959  M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\
    6060  M. Gaug\\ \texttt{<markus@ifae.es>} \\
    61   S. Mizobuchi\\ \texttt{<satoko@icrr.u-tokyo.ac.jp>}
     61  S. Mizobuchi\\ \texttt{<satoko@mppmu.mpg.de>}
    6262}
    6363
     
    167167\bibitem{ecl} Private communication with Lorenz E.
    168168
     169
     170%References used in Timing
     171\bibitem{DERISHEV} Derishev E.V., Kocharovsky V.V., Kocharovsky VI.V.,
     172AIP Conf.Proc.558:405-416,2001
     173
    169174%Not used references
    170175
  • trunk/MagicSoft/GRB-Proposal/Introduction.tex

    r6146 r6163  
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    77 \subsection{Observation of Soft Gamma Repeaters(SGRs)}
    78 A stronge magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' p
    79 eriodically emit gamma-ray, and  are extremely rare stars. Only four identified
    80 SGRs are discovered in the last 20 years: SGR0526-66, SGR1806-20, SGR1900+14, SG
    81 R1627-41. GRBs and SGRs can be explained with an unique precessing gamma jet mod
    82 el observed at different beam-angle and at different ages.
     77\subsection{Observation of SGRs}
     78A stronger magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' periodically emit gamma-ray, and are extremely rare stars. Only four identified
     79SGRs 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.\\
     80\par
     81The 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.\\
     82\par
     83MAGIC and Gamma-ray satellites react in the same way for also SGRs.
     84
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  • trunk/MagicSoft/GRB-Proposal/Timing.tex

    r6146 r6163  
    11\section{Timing considerations}
    22
    3 {\it Here, all possible models should go in with reasonning why certain time
    4 or flux estimates are proposed.  We have now only estimates on extrapolations
    5 of the \eg power-laws. Maybe we should include: IC (in many possible combinations), hadronic emission models (see~\cite{TASC}), Cannonball model.}
     3The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\
     4
     5%\subsection{Determine reasonable upper limit for observation duration }
     6According 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.\\
    67\par
     8For reprocessing of VHE Photons, the definition of minimal value B$_min$ is following.
     9\begin{equation}
     10B_{min} \sim \frac{5\times10^{-2}}{\Gamma^{3}}\,
     11             \frac{\epsilon_{2ph}}{1TeV}\,
     12             \frac{t_{GRB}}{10s}\, G
     13\label{eq:minimal}
     14\end{equation}
     15And the duration time of delay of reprocessed VHE emission may by calculated via the following function:
     16\begin{equation}
     17t_{d} \simeq \frac{2^{4/3}}{3} \biggl(\frac{B_{\perp}}{B_{min}}\biggl)^{2/3}
     18\label{eq:duration}
     19\end{equation}
     20When 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].\\
     21\par
     22In~\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.\\
     23\par
     24Li, 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).\\
     25\par
     26It 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.
    727
    8 The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\
    9 \par
    1028
    11 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.\\
    12 \par
    1329
    14 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).
    1530
    16 \par
    17 \ldots \textit{\bf UNTIL WHEN WILL WE OBSERVE THE BURST AFTER OCCURRANCE}   \ldots
    18 \par
    1931
    20 \subsection{Determine reasonable upper limit for observation duration }
     32
     33
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