Ignore:
Timestamp:
02/01/05 16:54:17 (20 years ago)
Author:
garcz
Message:
*** empty log message ***
Location:
trunk/MagicSoft/GRB-Proposal
Files:
2 edited

Legend:

Unmodified
Added
Removed
  • trunk/MagicSoft/GRB-Proposal/GRB_proposal_2005.tex

    r6175 r6176  
    129129\bibitem{ZHANG2} HE Spectral Components in GRB Afterglows,
    130130Zhang B., Meszaros P., Astrophys. J. 559, 110, 2001.
     131\bibitem{BELOBORODOV} Optical and GeV-TeV Flashes from GRBs, Beloborodov A., ApJ, 618, L13, 2005.
    131132\bibitem{EGRET} Hurley K. et al., Nature, 372, 652
    132133\bibitem{DINGUS} ESLAB29, Towards the Source of Gamma-Ray Bursts, Dingus, Ap\&SS, 231, 187, 1995.
    133 \bibitem{GONZALES} A GRB with high-energy Spectral Component Inconsistent with the Synchrotron Shock Model,
    134 Gonzales at al., Nature, 424, 749, 2003.
     134\bibitem{GONZALES} A GRB with high-energy Spectral Component Inconsistent with the Synchrotron Shock Model, Gonzales at al., Nature, 424, 749, 2003.
    135135\bibitem{AMENOMORI} Search for 10 TeV burst-like events coincident with the BATSE bursts
    136136using the TIBET Air Shower Array, Amenomori M., et al., A\&A, 311, 919, 1996.
  • trunk/MagicSoft/GRB-Proposal/Introduction.tex

    r6163 r6176  
    1212
    1313Very high energy (VHE) GRB observations have the potential to constrain the current GRB models
    14 on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}. 
    15 Models based on both internal and external shocks predicts VHE fluence comparable to, 
    16 or in certain situations stronger than, the keV-MeV radiation, 
     14on both the prompt and extended phases of GRB emission~\cite{HARTMANN,MANNHEIM,SALOMON}.
     15Models based on both internal and external shocks predicts VHE fluence comparable to,
     16or in certain situations stronger than, the keV-MeV radiation,
    1717with duration ranging from shorter than the keV-MeV burst to extended TeV afterglows~\cite{DERMER, PILLA, ZHANG1}.
    1818
    1919\par
    2020
    21 In many publications, the possibility that more energetic $\gamma$-rays come along with the 
    22 (low-energy) GRB, have been explored. Proton-synchrotron emission~\cite{TOTANI} have been suggested 
     21In many publications, the possibility that more energetic $\gamma$-rays come along with the
     22(low-energy) GRB, have been explored. Proton-synchrotron emission~\cite{TOTANI} have been suggested
    2323as well as photon-pion production~\cite{WAXMAN,BAHCALL,BOETTCHER} and inverse-Compton scattering
    2424in the burst environment~\cite{MESZAROS93,CHIANG,PILLA,ZHANG2}.
    25 Long-term HE $\gamma$ emission from accelerated protons in the forward-shock has been predicted in~\cite{LI}.
    26 This model predicts GeV inverse Compton emission even one day after the burst.
    27 Even considering pure electron-synchrotron radiation predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}.\\
     25Long-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.
     26Even considering pure electron-synchrotron radiation predicts measurable GeV emission for a significant fraction of GRBs~\cite{ZHANG2}. In order to be able to describe prompt synchrotron optical flashes (like observed in GRB990123 by ROTSE), GeV--TeV emission by inverse Compton scattering of the MeV photons should be produced at the same time~\cite{BELOBORODOV}.\\
    2827
    2928GeV emission in GRBs is particularly sensitive to the Lorentz factor and the photon density of the emitting material -
     
    3736The only significant detection was performed by \eg which detected seven GRBs emitting high energy (HE)
    3837photons in the 100\,MeV to 18\,GeV range~\cite{EGRET}. The data shows no evidence of a HE cut-off
    39 in the GRB spectrum~\cite{DINGUS}. Recent results indicate that the spectrum of some GRBs contains a very hard,
    40 luminous, long-duration component~\cite{GONZALES}.
     38in the GRB spectrum~\cite{DINGUS}. Recent results indicate that the spectrum of some GRBs contains a very hard, luminous, long-duration component~\cite{GONZALES}.
    4139There have been results suggesting gamma rays beyond the GeV range from the TIBET air shower array
    42 in coincidence with BATSE bursts~\cite{AMENOMORI}, rapid follow-up observations by the
    43 Whipple Air Cherenkov Telescope~\cite{CONNAUGHTON1}, and coincident and monitoring studies by HEGRA-AIROBICC~\cite{PADILLA},
    44 Whipple~\cite{CONNAUGHTON2} and the Milagro prototype Milagrito~\cite{MILAGRO}.
    45 The GRAND array has reported some excess of observed muons during seven BATSE bursts~\cite{GRAND}.
    46 In this context, especially the publication from the TASC detector on \eg is important~\cite{GONZALES},
    47 finding a HE spectral component presumably due to ultra-relativistic acceleration
    48 of hadrons and producing a spectral index of $-1$ with no cut-off up to the detector energy limit (200\,MeV).\\
     40in coincidence with BATSE bursts~\cite{AMENOMORI}, rapid follow-up observations by the
     41Whipple 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}. In this context, especially the publication from the TASC detector on \eg is important~\cite{GONZALES}, finding a HE spectral component presumably due to ultra-relativistic acceleration of hadrons and producing a spectral index of $-1$ with no cut-off up to the detector energy limit (200\,MeV).\\
    4942
    5043Concerning estimates about the \ma observability of GRBs, a very detailed study of GRB spectra obtained from the
     
    5548
    5649Taking into account the local rate of GRBs estimated in~\cite{GUETTA}, late afterglow emission from few tens of GRBs per year
    57 should be observable above our energy threshold. The model of~\cite{ASAF2} predict delayed GeV emission that
    58 should be significantly detectable by MAGIC in 100\,seconds.
     50should be observable above our energy threshold. The model of~\cite{ASAF2} predict delayed GeV emission that should be significantly detectable by MAGIC in 100\,seconds.
    5951
    6052\subsection{Observation of XRFs}
    6153
    6254While the major energy from the prompt GRBs is emitted in $\gamma$-rays ($E_p \sim$ 200~keV), XRFs are characterized
    63 by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties a connection between XRFs and GRBs is 
     55by peak energies below 50~keV and a dominant X-ray fluence. Because of similar properties a connection between XRFs and GRBs is
    6456suggested. The most popular theories say that XRFs are produced from GRBs observed ''off-axis''.
    65 Alternatively, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs. 
     57Alternatively, an increase of the baryon load within the fireball itself or low efficiency shocks can produce XRFs.
    6658If there is a connection between the XRFs and GRBs, they should originate at rather low redshifts (z $<$ 0.6).\\
    6759
    68 Gamma-ray satellites react in the same way to XRFs and GRBs. In case of a detection the coordinates are distributed 
     60Gamma-ray satellites react in the same way to XRFs and GRBs. In case of a detection the coordinates are distributed
    6961to other observatories (see section 2.1). Only from later analysis the difference can be established.
    7062
     
    7365In this case we include also the observation of XRFs by MAGIC in our proposal.
    7466
     67\subsection{Observation of SGRs}
    7568
     69Soft Gamma Repeaters (SGRs) are extremely rare strong magnetic neutron stars that periodically emit $\gamma$-rays. Only four identified SGRs were 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.\\
    7670
    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 
     71The BAT instrument on the SWIFT satellite triggered on an outburst from SGR1806-20 on 30. January 2005. The fluence was $\sim$ 1$\times$10$^{-5}$erg/cm$^2$(15-350keV). This event was five orders of magnitude smaller than the giant flare from this source on the 27. December 2004. If a giant flare from SGR occurs as SGR1806-20, MAGIC would be able to detect the 100\,seconds delayed $\gamma$-emission from the source.
Note: See TracChangeset for help on using the changeset viewer.