Changeset 6163 for trunk/MagicSoft
- Timestamp:
- 02/01/05 03:23:54 (20 years ago)
- Location:
- trunk/MagicSoft/GRB-Proposal
- Files:
-
- 3 edited
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trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex
r6162 r6163 59 59 M. Garczarczyk\\ \texttt{<garcz@mppmu.mpg.de>}\\ 60 60 M. Gaug\\ \texttt{<markus@ifae.es>} \\ 61 S. Mizobuchi\\ \texttt{<satoko@ icrr.u-tokyo.ac.jp>}61 S. Mizobuchi\\ \texttt{<satoko@mppmu.mpg.de>} 62 62 } 63 63 … … 167 167 \bibitem{ecl} Private communication with Lorenz E. 168 168 169 170 %References used in Timing 171 \bibitem{DERISHEV} Derishev E.V., Kocharovsky V.V., Kocharovsky VI.V., 172 AIP Conf.Proc.558:405-416,2001 173 169 174 %Not used references 170 175 -
trunk/MagicSoft/GRB-Proposal/Introduction.tex
r6146 r6163 75 75 76 76 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} 78 A stronger magnetic neutron star, a so-called ``Soft Gamma Repeaters (SGRs)'' periodically emit gamma-ray, and are extremely rare stars. Only four identified 79 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.\\ 80 \par 81 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.\\ 82 \par 83 MAGIC and Gamma-ray satellites react in the same way for also SGRs. 84 85 86 87 88 89 90 91 92 -
trunk/MagicSoft/GRB-Proposal/Timing.tex
r6146 r6163 1 1 \section{Timing considerations} 2 2 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.} 3 The 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 } 6 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.\\ 6 7 \par 8 For reprocessing of VHE Photons, the definition of minimal value B$_min$ is following. 9 \begin{equation} 10 B_{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} 15 And the duration time of delay of reprocessed VHE emission may by calculated via the following function: 16 \begin{equation} 17 t_{d} \simeq \frac{2^{4/3}}{3} \biggl(\frac{B_{\perp}}{B_{min}}\biggl)^{2/3} 18 \label{eq:duration} 19 \end{equation} 20 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].\\ 21 \par 22 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.\\ 23 \par 24 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).\\ 25 \par 26 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. 7 27 8 The EGRET~\cite{EGRET} instrument on the CGRO has detected GeV emission of GRB940217 promptly and 90 min. after the burst onset.\\9 \par10 28 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 \par13 29 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).15 30 16 \par17 \ldots \textit{\bf UNTIL WHEN WILL WE OBSERVE THE BURST AFTER OCCURRANCE} \ldots18 \par19 31 20 \subsection{Determine reasonable upper limit for observation duration } 32 33
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