Changeset 6120 for trunk/MagicSoft/GRB-Proposal/Introduction.tex

Timestamp:

01/29/05 17:38:13 (20 years ago)

Author:

gaug

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• trunk/MagicSoft/GRB-Proposal/Introduction.tex (modified) (4 diffs)

trunk/MagicSoft/GRB-Proposal/Introduction.tex

@@ -7 +7 @@
 the objective to turn the telescope to the burst position within 10-30\,sec.
 in order to have a fair chance to detect a burst when the emission is still ongoing.
-During the comissioning phase it could be proven that that goal was reached.
+During the commissioning phase it could be proven that that goal was reached.
 The telescope is able to turn 180 degrees in azimuth within 20\,sec. and 80 degrees in zenith within 10\,sec.\\
 
 
 Very high energy (VHE) GRB observations have the potential to constrain the current GRB models
-on both the prompt and extendend phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}. 
-Models based on both internal and external shocks predicts VHE fluence comperable to, 
+on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}. 
+Models based on both internal and external shocks predicts VHE fluence comparable to, 
 or in certain situations stronger than, the keV-MeV radiation, 
 with duration ranging from shorter than the keV-MeV burst to extended TeV afterglows~\cite{DERMER, PILLA, ZHANG1}.
@@ -24 +24 @@
 in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2}.
 Long-term HE $\gamma$ emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}. 
-This model predicts GeV inverse compton emission even one day after the burst.
+This model predicts GeV inverse Compton emission even one day after the burst.
 Even considering pure electron-synchrotron radiation predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}.\\
 
-GeV emission in GRBs is particulary sensitive to the Lorentz factor and the photon density of the emitting material - 
+GeV emission in GRBs is particularly sensitive to the Lorentz factor and the photon density of the emitting material - 
 and thus to the distance of the radiating shock from the source - due to the $\gamma~\gamma \rightarrow$
 \textit{e$^+$~e$^-$} absorption in the emission region. Direct comparison of the prompt GRB flux at $\sim$ 10\,GeV and $\sim$ 100\,keV 
@@ -37 +37 @@
 each indicating some excess over background but without stringent evidence. 
 The only significant detection was performed by EGRET which detected seven GRBs emitting high energy (HE) 
-photons in the 100\,MeV to 18\,dGeV range~\cite{EGRET}. The data shows no evidence of a HE rollover 
+photons in the 100\,MeV to 18\,dGeV range~\cite{EGRET}. The data shows no evidence of a HE roll-over 
 in the GRB spectrum~\cite{DINGUS}. Recent results indicate that the spectrum of some GRBs contains a very hard, 
 luminous, long-duration component~\cite{GONZALES}.
 There have been results suggesting gamma rays beyond the GeV range from the TIBET air shower array
 in coincidence with BATSE bursts~\cite{AMENOMORI}, rapid follow-up observations by the 
-Whipple Air Cerenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, 
+Whipple Air Cherenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA}, 
 Whipple~\cite{CONNAUGHTON2} and the Milagro prototype Milagrito~\cite{MILAGRO}.
 The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}. 
@@ -65 +65 @@
 by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties a connection between XRFs and GRBs is 
 suggested. The most popular theories say that XRFs are produced from GRBs observed ''off-axis''.
-Alternativly, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. 
+Alternatively, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. 
 If there is a connection between the XRFs and GRBs, they should originate at rather low redshifts (z $<$ 0.6).\\