Changeset 6146

Timestamp:

01/31/05 15:45:14 (20 years ago)

Author:

satoko

Message:

*** empty log message ***

Location:

trunk/MagicSoft/GRB-Proposal

Files:

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

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. 

trunk/MagicSoft/GRB-Proposal/Strategies.tex

@@ -6 +6 @@
 from the claimed GRB observation frequency  of about 150-200 GRBs/year by the SWIFT
 collaboration~\cite{SWIFT} and the results of the studies on the MAGIC duty-cycle 
-made by Nicola Galante~\cite{NICOLA} and Satoko Mizobuchi~\cite{SATOKO}.
+made by Nicola Galante~\cite{NICOLA}.
 Considering a MAGIC duty-cycle of about 10\% and a tolerance of 5 hours
 to point the GRB, we should be able to point about 1-2 GRB/month. 
@@ -20 +20 @@
 yet under observational control. 
 
-This reduction of the real duty-cycle w.r.t. the studies~\cite{NICOLA,SATOKO} 
+This reduction of the real duty-cycle w.r.t. the studies~\cite{NICOLA} 
 gets compensated by the tolerance of 5 hours for considering the alert observable 
 (5 hours more before the beginning of the night 

trunk/MagicSoft/GRB-Proposal/Timing.tex

@@ -1 +1 @@
 \section{Timing considerations}
 
-{\ldots \it \bf HAS TO BE UPDATED AND COMPLETED!! \ldots \\}
 {\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. }
+of the \eg power-laws. Maybe we should include: IC (in many possible combinations), hadronic emission models (see~\cite{TASC}), Cannonball model.}
 \par
 
-The EGRET~\cite{EGRET} instrument on the CGRO 
-has detected GeV emission of GRB940217 promptly and 90 min. after 
-the burst onset. 
-\\
+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. 
-\\
+
+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).
+
+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