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\title{Upward and Horizontal $\tau$ Airshowers by UHE Neutrinos}
%\title{Upward and Horizontal $\tau$ Airshowers by UHE $\nu$}

\author{\speaker{D.Fargion} \\
%        \thanks{Footnotes should appear on the
%        first page only to indicate your present address (if
%        different from your normal address), research grant,
%        sponsoring agency, alternative e-mail, etc. These are
%        obtained with the {\tt\ttbs thanks} command.}~

    Physics Department,INFN,Rome University 1,Italy\\
    E-mail: \email{daniele.fargion@roma1.infn.it}}
\received{\today}       %%
\revised{\today}
\accepted{\today}       %% These are for published papers.
%\JHEP{12(2001)999}     %%

\preprint{\hepth{9912999}}  % OR: \preprint{Aaaa/Mm/Yy\\Aaa-aa/Nnnnnn}
                % Use \hepth etc. also in bibliography.

\abstract{Upward and Horizontal $\tau$ Air-showers (UPTAUS and
HORTAUS) emerging from the Earth crust , mountain chains  or deep
plate boundaries are the most powerful signals of Ultra High
Energy UHE neutrinos $ \bar{\nu}_e $ at PeV and $\nu_{\tau}$,
$\bar\nu_{\tau}$ at energies  near and above $ 10^{15}-10^{19}
eV$. The large $\tau$  Air-showers multiplicity N in  secondaries
 $N_{opt} \simeq 10^{12} (E_{\tau} / PeV)$,
 $N_{\gamma} (< E_{\gamma} > \sim  10 \, MeV ) \simeq 10^8
(E_{\tau} / PeV)$, $N_{e^- e^+} \simeq 2 \cdot 10^7
(E_{\tau}/PeV)$, $N_{\mu} \simeq 3 \cdot 10^5
(E_{\tau}/PeV)^{0.85}$ make easy their discovery. UHE
$\nu_{\tau}$, $\nu_{\tau}$  because of neutrino flavor mixing,
($\nu_{\mu}\leftrightarrow \nu_{\tau}$),
 should be as abundant as $\nu_{\mu}$, $ \bar\nu_{\mu}$.
 Also $\bar{\nu}_e$, near the Glashow W resonance peak, $E_{\bar{\nu_e}} = M^2_W / 2m_e \simeq 6.3 \cdot
10^{15}\, eV$ may generate $\tau$ Air-showers. The HORTAUS may
test the UHE neutrino interactions  leading to additional
fine-tuned test of New TeV Physics  in  Mountain Valleys and
Earth crust  horizontal edges.  UPTAUS or HORTAUS, beaming toward
high mountains, air-planes, balloons and satellites should flash
 $\gamma$, $\mu$, X and Cherenkov lights toward detectors. Such
UPTAUS might already hit nearby most sensitive satellite as Gamma
Ray Observatory (GRO) detectors flashing them by short
(millisecond), hard, diluted $\gamma-$ burst at the edge of
threshold. We claimed their identity with the observed Burst And
Transient Source Experiment (BATSE) $78$ Terrestrial Gamma Flashes
(TGF). The TGF  clustering toward Galactic Center and Plane, known
galactic and extra-galactic sources strongly support their UHE
$\nu_{\tau}$ origin.} \keywords{UHE neutrino -$\tau$ air
shower-GZK} \dedicated{Dedicated to Giorgio Perlasca  heroic acts
in Budapest, 1944}
\begin{document}
 It is well known that Ultra High Energy $UHE$ neutrino of astrophysical origin above tens TeV
might overcome the nearby noise vertical of secondary atmospheric
neutrinos. The latter, being secondaries of charged cosmic rays,
smeared by galactic magnetic fields, have lost their interesting
astrophysical source records. In  cubic kilometer underground
detectors, both ice or water, in order to avoid the noisy downward
atmospheric muons and to overcome the Earth opacity for vertical
upward tens-TeV neutrinos, one \cite{01} should better neglect
vertical signals and focus the attention mainly on Horizontal
Underground detectors in kilometers wide disk-like or ring-like
arrays finalized to trace horizontal UHE Muons and Taus ($10^{13}-
10^{18}eV$) born by UHE astrophysical $\nu_{\mu}$,$\nu_{\tau}$.
Moreover because of $\tau$ amplified showering we prefer to
suggest the UPTAUS and HORTAUS detection  (after their parental
UHE $(\nu_{\tau},\bar{\nu}_{\tau}) + N$ interactions in rock, the
$\tau$ ejection in air and their fast decay in flight) as the best
tool for UHE neutrino discovery.
\FIGURE{\epsfig{file=Fig5-01.eps,width=0.6\textwidth }
        \caption[]{The  UHE neutrino
    ranges as a function of the incoming UHE neutrino energy in Earth with
    overlapping the resonant $\bar{\nu}_e e$, $\nu_{\tau} N$ interactions;
    below  in the corner the growing UHE $\tau$ boosted Lorentz  range $R_{tau}$
     at the  same energies and in water lowest curve bounded by photo-pion interactions.
      Finally the solid line $R_{New}$  shows the interaction length due to New physics (extra dimension Gravity)
    at TeV for a matter density of rock $\rho =3$.\cite {01}, \cite {02}}%
    \label{Fig001}}
    Indeed UHE $\nu_{\tau}$ and $\bar{\nu_{\tau}}$ may be flavor
converted from common pion secondaries: $\nu_{\mu}$ and
$\bar{\nu_{\mu}}$. The UHE neutrinos $\bar{\nu_e}$,
${\nu}_{\mu}$, $\bar{\nu}_{\mu}$, are expected Ultra High Energy
Cosmic Rays  (UHECR) ( $\gtrsim 10^{16}$ eV) secondary products
near Active Galactic Nuclei (AGN) or micro-quasars jets by common
photo-pion decay relics by optical photons nearby the source,
either pulsars (PSR) or AGNs ($p + \gamma \rightarrow n + \pi^+,
\pi^+ \rightarrow \mu^+ \nu_{\mu}, \mu^+ \rightarrow e^+ \nu_e
\bar{\nu}_{\mu} $), or directly by proton proton scattering in
interstellar matter. UHE  neutrino  flavor  mix even at highest
Greisen-Zatsepin-Kuzmin (GZK) energy ($ > 4\cdot 10^{19} eV$)
because of the large galactic (Kpcs) and extreme cosmic (Mpcs)
distances much longer than oscillation ones:
 \begin{equation}
 L_{\nu_{\mu} - \nu_{\tau}} = 4 \cdot 10^{-3} \,pc \left(
 \frac{E_{\nu}}{10^{16}\,eV} \right) \cdot \left( \frac{\Delta m_{ij}^2
 }{(10^{-2} \,eV)^2} \right)^{-1}
 \end{equation}
  HORTAUS  are better detectable in deep valleys or on front
 of large mountain chains  like Alps, Rocky Mountains, Grand Canyons, Himalaya
  and Ande just near present AUGER project \cite{03},\cite{05}. Future Array
  Telescope may trace at best such EeV ($10^{18}$
 eV) HORTAUs in  the Death
 Valley in USA by photoluminescent tracks \cite{04}. The mountain chains screens undesirable  horizontal
$(>70^o)$ UHECR showers; HORTAUS may   lead also to UHE
horizontal muon bundle. The Mountain chains acts also as a
characteristic  $\bar{\nu_e}$ detector  at Glashow energy peak ($
6.3 PeV$). Present UPTAUS   is analogous to the  well-known
\cite{06}  " $\tau $ double bang". The novelty lays in the
explosive $\tau$ decay in air after its escape from the rock leading to amplified tau air-showers
in flight. The UPTAUS-HORTAUS channels  reflects the known  $\tau$ decay modes (Fig.2). %\\

%%\begin{figure}[h]
%%%\includegraphics[width=7.0cm,height4=cm]{TableTau2.eps} %
%%\begin{center}
%%\includegraphics[width=0.80\textwidth]{TableTau1.eps} %
%%\end{center} \caption{The characteristic decay channels of UPTAUS and HORTAUS.}
%%\end{figure}
\FIGURE{\epsfig{file=TableTau1.eps,width=0.8\textwidth }
        \caption[]{The characteristic decay channels of UPTAUS and HORTAUS.}%
%    \label{Fig001}
}

From the top of a mountain, a balloon or a satellite  the Earth
acts also as a huge target for UPTAUS or its wide corona crust for
HORTAUS. Observing from a height h downward toward the Earth at
any angle $\theta$ below the horizontal line,($\theta$ +$\pi/2$ =
zenith angle), the distances $d{(\theta)}$ toward the ground,
(from where an UPTAUS or HORTAUS should arise) is:
 \begin{equation}
 d{(\theta)}= (R_{\oplus}+ h) \cdot \sin\theta -
 \sqrt{(R_{\oplus}+ h)^{2}\cdot \sin^{2}\theta -(2hR_{\oplus} + h^2 )}
 \end{equation}
The distance length at horizontal tangential angle $\theta_{c}$
where the square-root term above vanishes, simplify in:
\begin{equation}
d{(\theta_{c})} = \sqrt{(2 R_{\oplus}\cdot h)+ h^2}\simeq
110\sqrt{ \frac{h}{km} }\cdot km
 \end{equation}
Where $\theta_{c} = \arcsin \sqrt{(2 h/ R_{\oplus})}\simeq 1.01
^\circ \sqrt{(h/km) }$; the terrestrial cord  distances
$\bigtriangleup d{(\theta)}$ crossed by the primary UHE
$\nu_{\tau}$ (and partially by the consequent upcoming $\tau$
before its exit in air) is
\begin{equation}
 \bigtriangleup d{(\theta)}= 2
  \sqrt{(R_{\oplus}+ h)^{2}\cdot \sin^{2}\theta -(2hR_{\oplus} + h^2 )}
 \end{equation}
 Such distances, which vanish for $\theta =\theta_{c}$, are not too long
 to suppress horizontal UHE neutrinos for small  $\delta\theta$ ($= \theta-\theta_c$) angles above $\theta_{c}$,
  even at energies $E_{GZK}$  $ \simeq 4 \cdot 10^{19} eV$ energies. see Fig 1. The  $\nu_{\tau}$+${\tau}$ crossed distances are $ \bigtriangleup
  d(\delta\theta)$:
\begin{equation}
 \bigtriangleup d{(\delta\theta)}\simeq 2(R_{\oplus}+ h)
  \sqrt{\delta\theta \sin 2\theta_c }\simeq  318 km \sqrt {\left(
 \frac{\delta\theta}{1^{\circ}} \right) \sqrt {\left(
 \frac{h}{km }\right)}}
 \end{equation}
 The  terrestrial surface below any high level observer covers huge areas
  A  ($ A = 2\pi R_{\oplus} (1-cos(\theta_c)) \simeq 2 \pi h  R_{\oplus} \simeq 4\cdot 10^4 \cdot km^2 (h/km)$ for $h <<
  R_{\oplus}$); however for too distant UPTAUS  origination the shower signal might be bounded by
   the longer crossed slant depth atmosphere opacity.  The effective  area for UPTAUS observed from height h $ > h_\circ$
  ($h_\circ$ is the atmosphere exponential length $\simeq 8.55 km$ ) is  smaller:
  $A_{eff} = \pi \cdot \cot^2(\theta) h^2 = 942 \cdot km^2 (h/ 10 \cdot km)^2; (\theta= 60^\circ).$
  The Tau decay track (see the line $R_{\tau}$ in Fig.1), constrained by  the characteristic distance horizons $d{(\theta_{c})}$
  defines a fine tuned HORTAU energy: $E_{\tau} = 2\cdot 10^{18} eV \sqrt{(h/km)}$. This formulas cannot be extended to arbitrary
  energy (or any height h), because of the finite atmosphere size; see
  below. A too large tau lifetime may lead to $\tau$ decay in too empty
  atmosphere.
% Moreover the consequent ultra-relativistic  ($E_{\bar{\nu_{\tau}}} \geq 10^{17} - 10^{19}$ eV)
%  tau may travel in atmosphere for few or even hundred $kms$
%   with no absorption before the decay  to the detector located at few kms distance.
%    On the contrary  the horizontal gamma, electron pairs and
%     muon showers by primary (down-ward nearly horizontal)
%   UHECR proton  are severely suppressed   ($\leq 10^{-3}$) after
%   crossing  $(\geq 2\cdot 10^{3}\,g \cdot cm^{-2})$ slant depth, or equivalent at one
%   atmosphere,  ($\geq 16 kms $) of horizontal atmosphere target.
 Keeping care of the Earth opacity, at large nadir angle ($\gtrsim {60}^0$)
where an average Earth density may be assumed ($< \rho > \sim 5$)
the transmission probability and creation of upward UHE $\tau$ is
approximately:
\begin{equation}
P(\theta,\, E_{\nu}) = e^{\frac{- \bigtriangleup
d{(\theta)}}{R_{\nu_{\tau}}(E_{\nu})}} (1 - e^{-
\frac{R_{\tau}(E_{\tau})}{R_{\nu_{\tau}}(E_{\nu})}}) \, .
\end{equation}
This expression should contain $\bigtriangleup d{(\theta)}$ from
above equation and the ranges $R_{\nu_{\tau}}$ and $R_{\tau}$
\cite{01}are shown in Fig 1; for example at PeV the  above
probability is within a fraction of a
million(${\theta}{\approx}{60}{^0}$) to a tenth of thousands
(${\theta}{\approx}{\theta_c}$). At GZK energies only HORTAUS are
allowed. The corresponding angular integral effective volume
observable from a high mountain (or balloon) at height $h$
(assuming a final target terrestrial density $\rho = 3$) for
UPTAUS at 3 PeV (for any  AGN neutrino flux model
  normalized within a  flat spectra whose
energy fluence $ \phi_{\nu}\simeq 2 \,10^{3} \frac{eV}{cm^{2}\cdot
s}$), is:
\begin{footnotesize}
\begin{equation}
  V_{eff} \approx 0.3 \, km^3 \ffrac{\rho}{3}\ffrac{h}{km} e^{-
  \ffrac{E}{3\,PeV}}
  \ffrac{E}{3\,PeV}^{1.363}
\ffrac {\phi_{\nu}}{2 \,10^{3}\frac{eV}{cm^{2}\cdot s}}
\end{equation}
\end{footnotesize}
 Any  AGN neutrino flux model
  normalized within such a  flat spectra
is leading, above 3 PeV, to $\sim$ 10 UHE $\nu_{\tau}$ upward
event/km$^3$ year \cite{02}. The consequent average upward
effective event rate  on a top of a mountain (h $\sim 2\,km$) is:
\begin{footnotesize}
\begin{equation}
  N_{eff} \simeq 8 \, \frac{\mathrm{events}}{\mathrm{year}} \ffrac{\rho}{3} \ffrac{h}{2 \,km}
e^{- \ffrac{E}{3\,PeV}} \ffrac{E}{3\,PeV}^{1.363} \ffrac
{\phi_{\nu}}{2 \,10^{3}\frac{eV}{cm^{2}\cdot s}}
\end{equation}
\end{footnotesize}
Their signals at ten kms distances should be $\phi_{\gamma} \simeq
10^{-4} \div 10^{-5} cm^{-2} s^{-1}$, $(\phi_{X \sim 10^5 eV})
\simeq 10^{-2} \div 10^{-3}cm^{-2} s^{-1})$. The optical
Cherenkov flux is large $\Phi_{opt} \approx 1 cm^{-2}$.
%\section{Upward $\tau$ Air Shower in Terrestrial Gamma Flash: evidences of UHE neutrinos?}
%The tau upward air showers born in a narrow energy
% window, $10^{15}$ eV $ \lesssim E_{\nu} \lesssim  5 \cdot 10^{16} $
% eV (Fig.3) may penetrate high altitude leaving rare beamed upward gamma
%% shower bursts whose sharp ($\sim $ hundreds $\mu$sec because of the hundred kms high
 %altitude shower distances) time
 %structure and whose hard ($\gtrsim 10^{5}$eV) spectra may hit near
 %terrestrial satellites.
We claimed \cite {01} that such UPTAUS or HORTAUS produce gamma
bursts at the edge of GRO-BATSE  originated from the Earth and
named consequently as Terrestrial Gamma Flashes (TGF).
%The visible Earth surface from a satellite, like BATSE, at
%height $h \sim 400$ km and the consequent effective volume for
%UHE $\nu_{\tau} N$ PeVs interaction and $\tau$ air shower beamed
%within $\Delta \Omega \sim 2 \cdot 10^{-5} rad^2$ is: (note
%$<\rho> \simeq 1.6$ because 70 \% of the Earth is covered by seas)
%\begin{equation}
 %$ V_{eff} = V_{TOT} \Delta \Omega \simeq 60 \, km^3.$
%\end{equation}
The effective volume for UPTAUS and the event rate within an angle
of view ($\theta> 60^o$) is, at 3 PeV,  approximately to within 15
km$^3$ values and the expected UHE PeV  rate is:
\begin{equation}
  N_{ev} \sim 150 \cdot e^{-
  \ffrac{E_\tau}{3\,PeV}}
  \ffrac{E_\tau}{3\,PeV}^{1.363}% (E_\tau \sim 3 \mathrm{PeV})
  \ffrac{h}{400 km} \,
  \ffrac {\phi_{\nu}}{2 \,10^{3}\frac{eV}{cm^{2}\cdot s}}
  \frac{\mathrm{events}}{\mathrm{year}}
\end{equation}
The TGF signals would be mainly $\gamma$ at flux $10^{-2}$
cm$^{-2}$ at X hundred keV energies.
 The correlations of these clustered TGFs directions
 toward   GeV-MeV (EGRET), X  sources, Milky Way Galactic Plane (Fig.3)  support
 and make suggestive the TGF  identification as UPTAUS and HORTAUS. The TGF location reflects the higher UPTAUS (and HORTAUS)
 interaction probability in the rock  over the sea (and along the
coastal plates). Highest magnetic field on Asia  widely spreads
UPTAUS  making the TGF more observable. The present TGF-$\tau$
could not  be produced by UHE $\bar{\nu}_e$  because of the
severe Earth opacity and support the $\nu_{\mu}\leftrightarrow
\nu_{\tau}$  flavor mixing.
   %  At the present the very probable $\nu_{\tau}
   %  \bar{\nu_{\tau}}$ source of TGFs and their probable partial galactic location
   %  infer a first lower bound on
   %  $\Delta_{m_{\nu_{\mu} \nu_{\tau}}}$ ($L < 4$ Kpc, $\Delta_{m_{\nu_{\mu} \nu_{\tau}}}
   %   > 10^{-8}$ eV$^2$)
   %  and it offers a first direct test of
   %  the same existence of the last evanescent (hardly observed only recently),
   %  fundamental neutral lepton  particle: $\nu_{\tau}$ and $ \bar{\nu_{\tau}}$.
     The new physics interaction at TeV while forbid upward UHE signals in
     underground $km^3$ detectors it will amplify the $\nu_{\tau}$ signals
     beyond mountains,  by two order of magnitude making extremely fruit-full
     UHE $\nu_{\tau}$ astrophysics in near future.
\FIGURE{\epsfig{file=Fig6.eps,width=0.8\textwidth }
        \caption[]{ TGF events toward galactic center, disk and known
 sources on EeV AGASA map. Four red cross mark last TGF events. \cite{01}.}%
    \label{Fig003}}
  HORTAUS may develop nor at too dense low atmosphere (being absorbed), neither at too high, low atmosphere
(where no shower may be amplified). HORTAUS charged secondaries
may also turn upward by geo-magnetic fields into fan-thin- cone
jets, appearing as UPTAUS. The maximal $c\tau$ distance is ruled
by:
\begin{equation}\label{13}
  \int_{0}^{+ \infty} n_0 e^{-\frac{\sqrt{(c\tau+x)^2+R_\oplus^2} - R_\oplus}{h_0}}
   dx \cong  \int_{0}^{+ \infty} n_0 e^{-\frac{(c\tau+x)^2} {2h_0R_\oplus}}
   dx \cong n_0 h_0 A
\end{equation}
\begin{equation}\label{15}
%  c\tau = \sqrt{2R_\oplus h_0}
%  \sqrt{ ln \ffrac{R_\oplus}{c\tau} - ln A \left(1+\alpha \cdot ln
%  \ffrac{E}{E_{max}}\right)}
 c\tau = \sqrt{2R_\oplus h_0}
 \sqrt{ln \ffrac{R_\oplus}{c\tau} - ln A }
\end{equation}
Where $A=A_{Had.}$ or $A=A_{\gamma}$ are parameters of order of
unity, logarithmic function of energy,  that calibrate the energy
shower slant depth for both hadronic or electro-magnetic
nature,\cite{04}: $A_{Had.}=0.792 \left[1+0.02523
 \ln\ffrac{E}{10^{19}eV}\right];$
  $A_{\gamma}=\left[1+0.04343\ln\ffrac{E}{10^{19}eV}\right].$
The solution of this equation leads to a characteristic UHE
$c\tau_{\tau}$ = $546 \;km$ decay distance  at height $h= 23$ km
where the HORTAUS start to shower. This imply a possibility to
discover efficiently by satellite and balloons arrays  UHE
$\nu_{\tau}$, $\bar\nu_{\tau}$ up to $1.11$ $10^{19}eV $.
\cite{04,07}. From high satellite  the arrival HORTAUS angle maybe
confused ($\mp  1^\circ$) with most common Albedo Horizontal High
Altitude Showers (HIAS) \cite{04}. However from balloons heights
and below, HIAS  arrival angles split ($\geq 7^\circ$) from
HORTAUS ones and are well  distinguished. There is also the
simplest possibility to observe UPTAUS and HORTAUS while they are
hitting and lightening, via Cherenkov lights, upward mountain
snow-walls. Such UPTAUS may also beam on lower boundary of high
altitude clouds in the nights. These reflected flashing lights
have a characteristic twin beam eight-shaped imprint that offers
to Telescopes a new kind of signature for UHE Neutrino
Astrophysics.


%%%\begin{figure}[bt]
%%%\begin{center}
%%%% \mpicplace{9 cm}{3 cm}
%%%%\includegraphics[width=0.9\textwidth , height=7.0cm]
%%%\includegraphics[width=0.45\textwidth]
%%%{Fig6.eps}
%%%  \caption {The TGF on EGRET map. The TGF clustering toward the galactic center and known
%%%  EGRET sources, their squeezing along the Galactic Plane make them probably of astrophysical
%%%  nature.}
%%%\end{center}
%%%    \label{fig:boxed_graphic 5}
%%%\end{figure}

%%%\begin{acknowledgements}
%%%The author thanks P.G. De Sanctis Lucentini.  for technical support.
%%%\end{acknowledgements}

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\bibitem{02} R. Gandhi, C. Quigg, M.H. Reno, I. Sarcevic: Phys. Rev. D {\bf 58}, 093009 (1998)
\bibitem{03} D. Fargion, A. Aiello, R. Conversano, 26th ICRC, He6.1.09,p.396-398.1999.(USA);
\bibitem{04} D. Fargion,  27th ICRC 2001, HE1.8,Vol-2, Pag. 903-906, 2001.(Germany).
\bibitem{05} X. Bertou et all,astro-ph/0104452.
\bibitem{06} J. G. Learned, S. Pakvasa: Astropart. Phys. {\bf 3}, 267 (1995)
\bibitem{07} D. Fargion, A. Salis, B. Mele: Ap. J. {\bf 517}, 725--733(1999),USA.
% \bibitem{3} J. G. Learned, S. Pakvasa: Astropart. Phys. {\bf 3}, pp. 267 (1995)

%Ref 02%
%\bibitem{02} R. Gandhi, C. Quigg, M.H. Reno, I. Sarcevic: Phys. Rev. D {\bf 58}, 093009 (1998)

%Ref 03%
%\bibitem{11}  D. Fargion, A. Salis: In: {\it Proc. 25th ICRC, Salt Lake City, 1997}, HE-4-6 (1997) pp.~153--156


%\bibitem{16} D. Fargion, A. Salis, B. Mele: Ap. J. {\bf 517}, pp. 725--733 (1999), astro-ph/9710029

%Ref 05%
%\bibitem{17} D. Fargion: Lett. Nuovo Cimento {\bf 31}, 499 (1981)
%\bibitem{17} D. Fargion: Lett. Nuovo Cimento {\bf 31}, pp. 499 (1981)

%Ref 06%
%\bibitem{18} D. Fargion: Nuovo Cimento
%{\bf 65B}, 316 (1981) F. Antonelli, R. Konoplich, D.~Fargion: Lett. Nuovo Cimento {\bf 32}, 289 (1981)

%\bibitem{18} D. Fargion: Nuovo Cimento
%{\bf 65B}, pp. 316 (1981) F. Antonelli, R. Konoplich, D.~Fargion: Lett. Nuovo Cimento {\bf 32}, pp. 289 (1981)


%Ref 07%
%\bibitem{19} D. Fargion: Nuovo Cimento {\bf 77B}, 111 (1983)
% \bibitem{19} D. Fargion: Nuovo Cimento {\bf 77B}, pp. 111 (1983)

%Ref 08%

%Ref 09%
%\bibitem{24} D. Fargion: astro-ph/0002453, (2000); astro-ph/0005439.(2000)

     %Ref 10%
%\bibitem{27} Y.N. Hayashida et al.: In: {\it Proc. 26th ICRC, Salt Lake City, 1999}, OG.1.3.04


%%%%\bibitem{proc} F. Nesti and P. Dall'Aglio, \emph{Sample proceedings in
%%%%        JHEP format}, SISSA 2001.
%%%%\bibitem{fltf}  Maths Dahlgren, {\it Package {\tt floatflt}, distributed
%%%%        with \LaTeXe{} 96/06/01}, 1994-1996.
%%%%\bibitem{LC}    M. Goossens, F. Mittelbach, A. Samarin,
%%%%                {\it The \LaTeX{} Companion}, Addison-Wesley 1994.
%%%%\bibitem{TeXbook} D. E. Knuth, {\it The \TeX book}, Addison-Wesley 1986.


\end{thebibliography}


\end{document}



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%%%%%document, and sending e-mail.
%%%%%
%%%%%{\tt JHEP3.cls} has been developed to run on a version of \LaTeXe{}
%%%%%newer than or equal to {\bf `June 96'}, for code compatibility.
%%%%%
%%%%%\paragraph{New features in this release of {\tt JHEP3.cls}.}
%%%%%
%%%%%Besides the correction of some bugs, and the modifications to internal
%%%%%commands, there are some changes. The main ones concern the {\tt
%%%%%proceedings} option which is treated in~\cite{proc}. As for the journal
%%%%%style, the font has been reduced to {\tt 11pt}. The package {\sf
%%%%%amssymb} is used by default: this provides some special commands (like
%%%%%\verb!\gtrsim!  $\gtrsim$ and \verb!\lesssim! $\lesssim$) and the
%%%%%fonts \verb!\mathbb! to produce $\mathbb{R}$, $\mathbb{Z}$ and so on.
%%%%%More shortcuts for journals and archives have been added (see
%%%%%appendix~\ref{sec:A}). The bibliography is written ragged right to
%%%%%avoid frequent underfull boxes. Cross references can also, at need, be
%%%%%included in the abstract.
%%%%%
%%%%%
%%%%%\section{Syntax}
%%%%%
%%%%%
%%%%%% DO NOT LOOK AT THE FOLLOWING, IT'S PARTICULAR, DUE TO \tt.
%%%%%\TABLE{\footnotesize\fbox{\parbox{7.2cm}{\baselineskip .7\baselineskip\tt\noindent
%%%%%                    \let\lbr\{\def\{{\char'173}%
%%%%%                          \def\}{\char'175}%
%%%%%    \smallskip\ttbs documentclass[options]\{JHEP3\}\\
%%%%%    \ttbs title\{...\}\\
%%%%%    \ttbs author\{name1\ttbs\ttbs\ addr\ttbs\ttbs\ E-mail:\ \ttbs email\{...\}\}\\
%%%%%    \ttbs author\{name2\ttbs\ttbs\ addr\ttbs\ttbs\ E-mail:\ \ttbs email\{...\}\}\\
%%%%%    \ttbs abstract\{...\}\\
%%%%%    \ttbs keywords\{...\}\\[-1ex]
%%%%%    \ttbs preprint\{...\}\rm\ or
%%%%%    \tt$\left\lbr\hskip-1.2ex\hbox{\tt\begin{tabular}{l}
%%%%%    \ttbs received\{...\}\\
%%%%%    \ttbs revised\{...\}\\
%%%%%    \ttbs accepted\{...\}\\
%%%%%    \ttbs JHEP\{...\}\end{tabular}}\right.$\\[-1ex]
%%%%%    \ttbs dedicated\{...\}\\
%%%%%    \vdots\\
%%%%%    \ttbs begin\{document\}\\
%%%%%    \vdots\\
%%%%%    \ttbs acknowledgments\\
%%%%%    \vdots\\
%%%%%    \ttbs end\{document\}
%%%%%    }\caption[Structure of a document]{Structure of a document}}}
%%%%%
%%%%%
%%%%%The {\sf JHEP} class has just a minor number of differences
%%%%%compared to the standard {\sf article} of \LaTeX, as well as some new
%%%%%features. This table shows the structure of a document.
%%%%%
%%%%%The first command declares that you are using the {\sf JHEP} class,
%%%%%and provides the desired \textref{options}{options}.
%%%%%
%%%%%Then \verb!\title!, \verb!\author!, \verb!\abstract! are
%%%%%required for the \textref{titlepage}{title page} contents.
%%%%%
%%%%%A command \verb!\preprint! is active to insert the
%%%%%preprint numbers at the top right-hand corner, unless
%%%%%the \textref{published}{{\tt published} option} is provided.
%%%%%
%%%%%In this case the paper is assumed to be accepted for publication in JHEP and
%%%%%its history must be supplied with the  commands \verb!\received!,
%%%%%(possibly \verb!\revised!), \verb!\accepted!, \verb!\JHEP!.
%%%%%
%%%%%At \verb!\begin{document}! a title page is automatically generated
%%%%%so that there is no need for a \verb!\maketitle! command, or
%%%%%{\tt titlepage} option.
%%%%%
%%%%%An \verb!\acknowledgments! command can be used to insert the
%%%%%relative section, in its place, e.g. at the end of the introduction or after
%%%%%the conclusions.
%%%%%
%%%%%
%%%%%\section{Options}
%%%%%The following table shows the options which can be used
%%%%%at the \verb!\documentclass! command for {\sf JHEP}:
%%%%%
%%%%%\TABULAR[t]{|l|l|}{\hline
%%%%%\tt hyper(*),
%%%%%        & To choose between hyper and paper versions.\\
%%%%%\tt nohyper $\equiv$ paper
%%%%%        & Hyper version is hyper-active and oneside.\\
%%%%%        & Paper version is not hyper-active.\\
%%%%%\hline
%%%%%\tt draft   & Enables the draft mode: labels and citations appear on\\
%%%%%        & the margin, processing info at the top of every page,\\
%%%%%        & and {\tt epsfig} figures appear as a box with the filename. \\
%%%%%\hline
%%%%%\tt a4paper(*), & Standard paper size options. \\
%%%%%\tt letterpaper & Options {\tt a5paper, b5paper, landscape}\\
%%%%%\tt legalpaper  & are not defined.\\
%%%%%\tt executivepaper  &\\
%%%%%\hline
%%%%%\tt 11pt, 12pt(*)& For preprints only, the author can choose {\tt11pt}
%%%%%            or {\tt 12pt}.\\
%%%%%\hline
%%%%%\tt oneside(*), twoside
%%%%%    & These set the page margins for one or two-side mode \\
%%%%%    & and the side of figures, tables and margin notes.\\
%%%%%\hline
%%%%%\tt notoc%
%%%%%        & To disable the automatic table of contents.\\
%%%%%\hline
%%%%%\tt published\label{published}%
%%%%%        & Inserted by the Journal for processing accepted papers.\\
%%%%%\hline}{Options\label{options}}
%%%%%
%%%%%Options with an asterisk ({\tt hyper, a4paper, 12pt, oneside}) are the
%%%%%default behavior. Note that {\tt titlepage, 10pt, a5paper, b5paper,
%%%%%landscape} are not provided. The option {\tt proceedings} to write
%%%%%contributions for congresses is described in~\cite{proc}.
%%%%%
%%%%%
%%%%%
%%%%%\section{Format}
%%%%%
%%%%%The following defaults are fixed as the selected format for publication and,
%%%%%accordingly, some \LaTeX{} commands and options are disabled.
%%%%%
%%%%%
%%%%%\subsection{Dimensions}
%%%%%
%%%%%The width and the height of the text depend on the declared
%%%%% paper type. They amount to 74\% of the paper width and 77\% of the
%%%%%paper height.
%%%%%
%%%%%The default is {\tt a4paper}, and the text dimensions are shown on
%%%%%these pages: width 15.5\,cm, height  22.8\,cm.
%%%%%
%%%%%The value of \verb!\baselinestretch! is set to 1.1 line spacing.
%%%%%
%%%%%
%%%%%\subsection{Pagestyle}
%%%%%
%%%%%The selected pagestyle is that of the present example and
%%%%%\verb!\pagestyle!, \verb!\thispagestyle! are ignored.
%%%%%
%%%%%
%%%%%\subsection{Fonts}
%%%%%
%%%%%The default font is a 11 point CM Roman, both for the hyper version
%%%%%than the paper one. This dimension is easy to read on the screen and
%%%%%is suitable for reduction. This is the only choice allowed for published
%%%%%papers.
%%%%%
%%%%%For preprint papers the author is free to choose a {\tt 11pt} or
%%%%%{\tt 12pt} option.
%%%%%
%%%%%
%%%%%\subsection{Equations} \label{sec:eq}
%%%%%
%%%%%Equations are formatted as in plain \LaTeX, plus hyperlinks, like in
%%%%%the example at the end of these pages (see equation~\ref{eq:pi}).
%%%%%The spacing around the {\tt\&}'s in the {\tt eqnarray} environment
%%%%%is slightly reduced, equal to that of the {\tt equation} environment.
%%%%%
%%%%%\subsection{Theorems and such}\label{sec:thm}
%%%%%
%%%%%The format for theorems, lemmas and so on is established. As usual they are to
%%%%%be defined by \verb!\newtheorem{theorem}{Theorem}!,
%%%%%\verb!\newtheorem{lemma}{Lemma}! \ldots. The command \verb!\Proof!
%%%%%is provided to introduce the proof.
%%%%%
%%%%%\subsection{Table of contents} \label{sec:toc}
%%%%%
%%%%%A table of contents is automatically inserted at the top of the second page,
%%%%%before the document starts. In case a document had no sections (e.g. letters or short
%%%%%communications) the table of contents is omitted.
%%%%%
%%%%%In preprint mode, the \textref{options}{{\tt notoc}} option can be given to
%%%%%suppress this behavior.
%%%%%
%%%%%
%%%%%\section{Title page}\label{titlepage}
%%%%%
%%%%%A title page is automatically generated at the beginning of the document,
%%%%%in `flushed left' style.
%%%%%Note that \verb!\maketitle! or the \verb!titlepage! option no longer exist.
%%%%%
%%%%%The top line contains either the preprint numbers
%%%%%or the JHEP logo, plus publication information, for papers accepted by the
%%%%%Journal.
%%%%%All the information on the title page is supplied with the following
%%%%%commands which must appear in the preamble.
%%%%%
%%%%%
%%%%%\subsection{Mandatory commands}
%%%%%\newcommand\bit{\noindent$\bullet$ \verb}
%%%%%
%%%%%\fverb!\title{...}!\fverbdo  The title, typeset in Sans-Serif.
%%%%%
%%%%%\fverb!\author{...\\...}!\fverbdo  This command provides the name of one
%%%%%or more authors.
%%%%%The lines after `\verb!\\!'  are typeset as the address,
%%%%%where line breaks can be obtained with further `\verb!\\!' commands.
%%%%%
%%%%%A single \verb!\author! should be used only for authors sharing the same
%%%%%address, while for other authors with different addresses more
%%%%%\verb!\author! commands can be used. The \textref{email}{\tt\ttbs email}
%%%%%command may be used (usually after the address) to provide e-mail link.
%%%%%
%%%%%\fverb!\abstract{...}!\fverbdo  This provides the abstract, and
%%%%%substitutes the old \LaTeX{} environment. By choice, only `horizontal'
%%%%%material can be put in the abstract, to prevent line breaks and
%%%%%display-math formul\ae. In-text formul\ae{} are of course allowed.
%%%%%Also note that the abstract is part of the title page and thus must be
%%%%%declared {\it before} \verb!\begin{document}!.
%%%%%
%%%%%

%%%%%\subsection{Optional commands}
%%%%%
%%%%%\fverb!\thanks{...}!\fverbdo  This command generates a footnote on
%%%%%the title page and should be used inside \verb!\author! to provide
%%%%%additional information for any single author, like research grants,
%%%%%sponsoring agencies, present address when different from the normal
%%%%%address, alternative e-mail addresses.
%%%%%
%%%%%\fverb!\preprint{...}!\fverbdo  This command is used to provide the
%%%%%preprint reference numbers. It inserts  this information at the top
%%%%%right-hand corner of the title page.
%%%%%
%%%%%\fverb!\keywords{...}!\fverbdo  This command inserts a line
%%%%%containing the keywords for the paper in question. A
%%%%%\href{http://jhep/JOURNAL/keywords.html}{list of
%%%%%keywords} is provided by the JHEP Journal. They must appear on
%%%%%the same line separated by commas.
%%%%%
%%%%%\fverb!\dedicated{...}!\fverbdo  This command inserts a dedication on the
%%%%%titlepage below the abstract, it is flushed right in small italic style.
%%%%%
%%%%%\fverb!\received{...}, \revised{...}, \accepted{...}, \JHEP{...}!\fverbdo
%%%%%
%%%%%\noindent These four commands should not be used by
%%%%%authors. They are automatically inserted by the Journal to show, in
%%%%%the head of the first page, the dates of arrival (revision) and
%%%%%acceptance, and to insert a `bop-hook' to show the vertical JHEP
%%%%%numbering in the published version.
%%%%%
%%%%%
%%%%%

%%%%%\section{Extra features}
%%%%%
%%%%%
%%%%%\subsection{Figures and tables}
%%%%%
%%%%%The {\sf JHEP} class can insert figures and tables in the text via the two
%%%%%basic commands:
%%%%%
%%%%%\marginpar{\small\sffamily FIGURE \ref{myfigure} . . called . . here.}
%%%%%
%%%%%\fverb!\FIGURE[pos]{body}!\fverbdo
%%%%%\smallskip
%%%%%\FIGURE{\epsfig{file=jhepfig.eps,width=5cm}
%%%%%        \caption[Example of figure]{Made with \tt\ttbs FIGURE.}%
%%%%%    \label{myfigure}}
%%%%%
%%%%%\noindent This command inserts an in-text figure like the example on the
%%%%%\csname if@twoside\endcsname\ifodd\count0left\else right\fi\else right\fi.
%%%%%The {\tt body} can contain any `horizontal' material, {\it i.e.\ no
%%%%%vskips}, and its width is automatically calculated.
%%%%%To select a given width one should enclose the content in a
%%%%%\verb!\parbox!.
%%%%%
%%%%%The \verb!\caption{...}! command can be used inside and works as usual.
%%%%%A typical form of {\tt body}, which uses {\sf epsfig},
%%%%%is `\verb!\epsfig{...}\caption{...}!',
%%%%%with any size changing commands.
%%%%%
%%%%%\medskip
%%%%%
%%%%%\fverb!\TABLE[pos]{body}!\fverbdo\smallskip\\
%%%%%This command is similar to \verb!\FIGURE!. As with the
%%%%%\verb!table! environment of \LaTeX{}, authors have to use a {\tt tabular}
%%%%%environment inside to generate the actual table.
%%%%%
%%%%%Both commands generate floating objects which are inserted in the

%%%%%text as soon as there is enough space on the page.
%%%%%If the object happens to be larger than 60\%{} of the textwidth,
%%%%%it is centered in the page like usual \LaTeX{} floats.
%%%%%
%%%%%%\marginpar{\small\sffamily Table \ref{mytable} . . called . . here.}
%%%%%
%%%%%\TABULAR{|c|l|}{
%%%%%    \hline  \tt r   & {\it right hand side}\\
%%%%%    \hline  \tt l   & {\it left hand side}\\
%%%%%    \hline  \tt p(*)& {\it right} in one-side mode\\
%%%%%            & {\it alternating} in two-side mode\\
%%%%%    \hline}{\label{mytable}Horizontal position as in \cite{fltf}}
%%%%%
%%%%%The optional argument {\tt pos} can be used to change the
%%%%%{\it horizontal} positioning, which by default is {\tt p}.
%%%%%This corresponds to: right hand side in one-side mode or
%%%%%outer part of the pages in two-side mode.
%%%%%
%%%%%Note that the side of pages is inverted with
%%%%%respect to usual numbering, due to the title page.
%%%%%
%%%%%In case the figure or table is larger than 60\%, the argument {\tt pos}
%%%%%selects the {\it vertical} positioning as in \LaTeX{} \cite{LC}, with the
%%%%%default setting {\tt ht}. As a consequence, by default, the big floats appear
%%%%%either at the point where they are called or at the top of subsequent pages.
%%%%%
%%%%%When in draft mode, if one wants a list of figures (or of tables) an
%%%%%optional argument to the caption should be added containiong the text
%%%%%due to appear in the list.

%%%%%
%%%%%Two further commands are provided as a shorthand for useful
%%%%%forms of \verb!\FIGURE! and \verb!\TABLE!:
%%%%%
%%%%%
%%%%%\fverb!\EPSFIGURE[pos]{filename}{capt}!\fverbdo\nopagebreak\smallskip\\
%%%%%\nopagebreak
%%%%%this command produces an in-text figure by calling the given {\it EPS
%%%%%file} with \verb!\epsfig!. It is equivalent to:
%%%%%\verb!\FIGURE[pos]{\epsfig{file=filename}\caption{capt}}!.
%%%%%
%%%%%Note that to use this command, the package {\sf epsfig} has to be invoked in the
%%%%%preamble with \verb!\usepackage{epsfig}!. Using {\sf epsfig} also
%%%%%gives the opportunity to scale the figures via the keywords {\tt
%%%%%width} or {\tt height}, e.g.:
%%%%%\verb!\EPSFIGURE[pos]{filename,width=...}{capt}!.
%%%%%
%%%%%
%%%%%\fverb!\TABULAR[pos]{align}{body}{capt}!\fverbdo\smallskip\\
%%%%%This command can be used to produce a complete table:
%%%%%{\tt align} represents the alignment directives as in the
%%%%%{\tt tabular} environment, {\tt body} contains the table entries, and
%%%%%{\tt capt} the table caption. This is equivalent to:\\
%%%%%\verb!\TABLE[pos]{\begin{tabular}{align}body\end{tabular}\caption{capt}}!
%%%%%
%%%%%
%%%%%\DOUBLEFIGURE[b]{jhepfig.eps, width=.4\textwidth}
%%%%%{jhepfig.eps, width=.4\textwidth}{caption 1}{caption 2}
%%%%%
%%%%%Moreover there are the commands
%%%%%
%%%%%\fverb!\DOUBLEFIGURE[pos]{filename1}{filename2}{capt1}{capt2}!\fverbdo\smallskip
%%%%%
%%%%%\noindent\fbox{\let\lbr\{\def\{{\char'173}\def\}{\char'175}%
%%%%%        \begin{tabular}{@{}l@{}l@{}}
%%%%%\tt\ttbs DOUBLETABLE[pos]&\tt\{\ttbs begin\{tabular\}...\ttbs end\{tabular\}\}\\
%%%%%&\tt\{\ttbs begin\{tabular\}...\ttbs end\{tabular\}\}\{capt1\}\{capt2\}\\
%%%%%      \end{tabular}}
%%%%%
%%%%%\noindent to put two figures (or tables) one besides the other each
%%%%%one with its caption and number.
%%%%%
%%%%%
%%%%%{\small
%%%%%The code to implement these features is a modification of the
%%%%%\LaTeXe{} package \verb!floatfig! \cite{LC}, still being developed
%%%%%(presumably?) under the new name \verb!floatflt! \cite{fltf}.
%%%%%
%%%%%The package has been modified to comply with JHEP requests and to
%%%%%correct the following problems: incompatibility with a \verb!\marginpar!;
%%%%%in two-side mode floats to the following page retained the
%%%%%previous (wrong) position; floats were not typeset at top of page.
%%%%%
%%%%%}% END SMALL.
%%%%%
%%%%%
%%%%%\subsection{Hyper-features}
%%%%%
%%%%%Unless the {\tt nohyper} option is issued (same as {\tt paper}) the
%%%%%following hyper-features are activated:
%%%%%
%%%%%\paragraph{Email.} \label{email} A new command:
%%%%%
%%%%%\fverb!\email{!\it user@address\verb!}!\fverbdo\\
%%%%%It inserts a {\tt mailto:user@address} link in the document to send
%%%%%directly e-mail to the author.
%%%%%The e-mail address is always typeset in \verb!tt! font.
%%%%%
%%%%%\paragraph{Href's.} There are three new commands:
%%%%%
%%%%%\fverb!\href{!\it link\verb!}{!text\verb!}!, \verb!\name{!tag\verb!}!,
%%%%%\verb!\base{!URL\verb!}!\fverbdo\smallskip\\
%%%%%The first two commands, the building blocks of hyperlinks, are
%%%%%equivalent to the HTML insertions \verb!<A HREF="link">text</A>!
%%%%%and \verb!<A NAME="tag"></A>!. The command \verb!\base! provides the
%%%%%base URL, used by some hyper-viewers to allow the use of relative
%%%%%URL's.
%%%%%Lastly, a control sequence \verb!\hash! which gives a \verb!#!, to be
%%%%%used inside \verb!\href! for linking manually inside documents.
%%%%%
%%%%%{\small(notice the absence of text inside the HTML tag, to make
%%%%%target anchors invisible and avoid hyper-nesting problems).}
%%%%%
%%%%%\paragraph{Table of contents.} The table of contents which appears on
%%%%%the second page contains hyperlinks to sections and pages.
%%%%%{\small(Because the TOC is not customizable, the code has to redefine
%%%%%internal \LaTeX{} commands, potentially breaking future compatibility).}
%%%%%
%%%%%\paragraph{Bibliography and citations.} Each \verb!\cite! carries a
%%%%%hyperlink to the respective item in the bibliography which appears at
%%%%%the end of the document. See for example \cite{TeXbook,LC}.
%%%%%{\small (As for the table of contents, compatibility is broken).} All
%%%%%references which use the provided \textref{sec:journ}{shortcuts}, are
%%%%%linked to the corresponding online data on JHEP, {\tt xxx} archives or SPIRES.
%%%%%
%%%%%\paragraph{Pages.} Every page carries a target \verb!NAME=pag!{\it n} at
%%%%%the top left corner.
%%%%%
%%%%%\paragraph{Refs.} In addition to the usual behavior, the three commands
%%%%%\verb!\label!, \verb!\ref!, \verb!\pageref! are hyper-active:
%%%%%\verb!\label{!{\it mylabel}\verb!}! inserts an HTML \verb!<A NAME=ref-mylabel>!
%%%%%tag into the text, again with zero width.
%%%%%The \verb!\ref{!{\it mylabel}\verb!}! command then carries a link to it.
%%%%%Also the \verb!\pageref{!{\it mylabel}\verb!}! command generates a
%%%%%link to the correct page
%%%%%(see the link to figure~\ref{myfigure} on page~\pageref{myfigure} or to
%%%%%eq.~\ref{eq:pi} on page~\pageref{eq:pi}). There is also a new command:
%%%%%
%%%%%\fverb!\textref{!\it mylabel\verb!}{!text\verb!}!\fverbdo\smallskip\\
%%%%%The argument {\it text} becomes a link to the given label. This can be used
%%%%%to produce HTML-like text links, but should be used sparingly, in view of the
%%%%%paper version. As an example of an internal link see the same
%%%%%\textref{myfigure}{picture}.
%%%%%
%%%%%If you have set your WWWBROWSER environment variable, or are running nDVI,
%%%%%you can follow the links to other documents. At present an external
%%%%%document can be called as a
%%%%%\href{http://babbage.sissa.it/dvi/hep-th/9702201}{whole},
%%%%%but in the future references to parts shall also be considered: for example
%%%%%a section like {\it``\href{http://babbage.sissa.it/dvi/hep-th/9702201\hash
%%%%%section.1}{Lightning review of string theory}''}.
%%%%%
%%%%%{\small We have chosen to refer to the label explicitly in the link
%%%%%to avoid problems with potentially dangerous redefinitions of
%%%%%equation numbers in \verb!\@currentlabel! (for example spaces).
%%%%%Note that in this way hyper-referencing across documents will require the
%%%%%knowledge of the original label name. }
%%%%%
%%%%%\subsection{Draft}
%%%%%
%%%%%The {\tt draft} mode provides the following features, in addition to
%%%%%the usual \csname if@draft\endcsname~~~~~~~~~~~~~\fi\verb!\overfullrule!:
%%%%%
%%%%%\paragraph{Processing info.} The heading shows various processing
%%%%%information: class options, job name, time and date of processing.
%%%%%
%%%%%\paragraph{Citations.} For each \verb!\cite! command the corresponding
%%%%%citation labels are reported in a margin note if possible, or locally.
%%%%%
%%%%%\paragraph{Labels.} At each \verb!\label! command the corresponding
%%%%%label is reported in the margin if possible, or locally.
%%%%%(See appendix~\ref{sec:flags}, eq.~\ref{eq:zero} or table~\ref{mytable}).
%%%%%
%%%%%\paragraph{List of figures (tables).} The commands
%%%%%\verb!\listoffigures! and \verb!\listoftables! work only in draft
%%%%%mode. If you use them you have to provide optional arguments to the
%%%%%captions the will appear in the lists.
%%%%%
%%%%%\subsection{Acknowledgments}
%%%%%
%%%%%\fverb!\acknowledgments!\fverbdo This command starts a new section where
%%%%%acknowledgments can be placed. It usually resides at the end of the
%%%%%introduction or at the end of the paper. In fact:
%%%%%
%%%%%\bigskip
%%%%%
%%%%%\acknowledgments
%%%%%
%%%%%For the present version {\sf JHEP 3.0}, we wish thank Simona Cerrato
%%%%%and the people at \href{http://www.sif.it}{SIF} (Societ\`a Italiana di
%%%%%Fisica) for advices regarding the typographical style. Still I shall
%%%%%thank Debora, human and linux at the same time. Also thanks to the entire JHEP staff.
%%%%%
%%%%%
%%%%%
%%%%%\appendix
%%%%%
%%%%%\section{Command summary}\label{sec:A}{\small
%%%%%
%%%%%\paragraph{Preamble commands.} Commands to build the
%%%%%\textref{titlepage}{title page}:
%%%%%
%%%%%\bit!\title{...}!: to declare the title.
%%%%%
%%%%%\bit!\author{names\\addr}!: to supply names of authors
%%%%%                and a single address. More commands must
%%%%%                be used for different addresses.
%%%%%                Further \verb!\\!'s in \verb!addr! can be used
%%%%%                to break lines in the address.
%%%%%
%%%%%\bit!\thanks{...}!: should be used inside \verb!\author! to
%%%%%            provide further information. It generates a
%%%%%            footnote in the titlepage.
%%%%%
%%%%%\bit!\abstract{...}!: provides the abstract.
%%%%%
%%%%%\bit!\preprint{...}!: provides the preprint numbers, which
%%%%%              are typeset in the upper right-hand corner.
%%%%%
%%%%%\bit!\keywords{...}!: provides the keywords, which appear
%%%%%              below the abstract. They are hyper-linked to the
%%%%%              appropriate search engine in JHEP. Separate with commas.
%%%%%
%%%%%\bit!\dedicated{...}!: a dedication is inserted on the
%%%%%               right hand-side, below the keywords.
%%%%%
%%%%%\paragraph{Tables and figures.} To generate floating tables and figures,
%%%%%                which are in-text if sufficiently
%%%%%                narrow.
%%%%%
%%%%%\bit!\TABLE[pos]{...}!: generates a table object.
%%%%%            It can be any `horizontal' material.
%%%%%            \verb!\caption! can be used inside it.
%%%%%
%%%%%\bit!\FIGURE[pos]{...}!: generates a floating in-text figure, similar to
%%%%%             \verb!\TABLE!.
%%%%%
%%%%%\bit!\TABULAR[pos]{align}{...}{capt}!: generates a full table, with
%%%%%                       \verb!align! are the column
%%%%%                       definitions as in \verb!tabular!,
%%%%%                       \verb!...! the table entries, and
%%%%%                       \verb!capt! the caption.
%%%%%
%%%%%\bit!\EPSFIGURE[pos]{filename}{capt}!: generates a figure from the
%%%%%                    EPS file \verb!filename!.
%%%%%
%%%%%\bit!\DOUBLETABLE[pos]{\begin{tabular}...\end{tabular}}!
%%%%%
%%%%%\hspace{6.7em}
%%%%%\verb!{\begin{tabular}...\end{tabular}}{capt1}{capt2}!:
%%%%%            produces two paired tables each with its caption
%%%%%            and number.
%%%%%
%%%%%\bit!\DOUBLEFIGURE[pos]{filename1}{filename2}{capt1}{capt2}!:
%%%%%            generates two paired figures each with its caption
%%%%%            and number.
%%%%%
%%%%%\paragraph{Hyper commands.}
%%%%%The usual \LaTeX commands for citations, labels, references, are
%%%%%hyper-active unless the {\tt nohyper} or {\tt paper} option is used to
%%%%%prepare the paper version. New specific commands are:
%%%%%
%%%%%\bit!\href{url}{text}!: this command
%%%%%can be used to link {\tt text} directly to some URL.
%%%%%
%%%%%\bit!\name{tag}!: in case the author wants to insert a personal HTML tag in the
%%%%%document.
%%%%%
%%%%%\bit!\base{url}!: some hyper-readers support relative URLs, and
%%%%%          \verb!\base! provides the base.
%%%%%
%%%%%\bit!\textref{label}{text}!: it is equivalent
%%%%%to the \verb!\ref! command; this
%%%%%links {\tt text} to the point where {\tt label} is used.
%%%%%
%%%%%
%%%%%\paragraph{Journals.}\label{sec:journ}
%%%%%The following shortcuts for high energy physics journals are provided, and
%%%%%authors are encouraged to use them. They all require three arguments which
%%%%%are, in order, the volume number, the year {\it(four digits)} and the page.
%%%%%For JHEP, the three arguments are: the month (two digits), the year (four
%%%%%digits) and the journal number (three digits).
%%%%%
%%%%%\setlength{\columnsep}{10pt}
%%%%%\begin{multicols}{2}\small
%%%%%\begin{verbatim}
%%%%%\apa   -> Acta Phys. Austriaca
%%%%%\apas  -> Acta Phys. Austriaca, Suppl.
%%%%%\appol -> Acta Phys. Polon.
%%%%%\advm  -> Adv. Math.
%%%%%\adnp  -> Adv. Nucl. Phys.
%%%%%\adp   -> Adv. Phys.
%%%%%\atmp  -> Adv. Theor. Math. Phys.
%%%%%\am    -> Ann. Math.
%%%%%\ap    -> Ann. Phys. (NY)
%%%%%\araa  -> Ann. Rev. Astron. & Astrophys.
%%%%%\arnps -> Ann. Rev. Nucl. Part. Sci.
%%%%%\asas  -> Astron. Astrophys.
%%%%%\asj   -> Astron. J.
%%%%%\app   -> Astropart. Phys.
%%%%%\apj   -> Astrophys. J.
%%%%%\baas  -> Bull. Am. Astron. Soc.
%%%%%\bams  -> Bull. Am. Math. Soc.
%%%%%\blms  -> Bull. London Math. Soc.
%%%%%\cjm   -> Can. J. Math.
%%%%%\cqg   -> Class. and Quant. Grav.
%%%%%\cmp   -> Comm. Math. Phys.
%%%%%\ctp   -> Comm. Theor. Phys.
%%%%%\cag   -> Commun. Anal. Geom.
%%%%%\cpam  -> Commun. Pure Appl. Math.
%%%%%\cpc   -> Comput. Phys. Commun.
%%%%%\dmj   -> Duke Math. J.
%%%%%\epjc  -> Eur. Phys. J. C
%%%%%\epjd  -> Eur. Phys. J. Direct. C
%%%%%\epl   -> Europhys. Lett.
%%%%%\forp  -> Fortschr. Phys.
%%%%%\faa   -> Funct. Anal. Appl.
%%%%%\grg   -> Gen. Rel. Grav.
%%%%%\hpa   -> Helv. Phys. Acta
%%%%%\ijmpa -> Int. J. Mod. Phys. A
%%%%%\ijmpb -> Int. J. Mod. Phys. B
%%%%%\ijmpc -> Int. J. Mod. Phys. C
%%%%%\ijmpd -> Int. J. Mod. Phys. D
%%%%%\ijtp  -> Int. J. Theor. Phys.
%%%%%\invm  -> Invent. Math.
%%%%%\jag   -> J. Alg. Geom.
%%%%%\jams  -> J. Am. Math. Soc.
%%%%%\jap   -> J. Appl. Phys.
%%%%%\jdg   -> J. Diff. Geom.
%%%%%\jgp   -> J. Geom. Phys.
%%%%%\jhep  -> J. High Energy Phys.

%%%%%\jmp   -> J. Math. Phys.
%%%%%\joth  -> J. Operator Theory
%%%%%\jpha  -> J. Phys. A
%%%%%\jphc  -> J. Phys. C
%%%%%\jphg  -> J. Phys. G
%%%%%\lmp   -> Lett. Math. Phys.
%%%%%\ncl   -> Lett. Nuovo Cim.
%%%%%\matan -> Math. Ann.
%%%%%\mussr -> Math. USSR Izv.
%%%%%\mams  -> Mem. Am. Math. Soc.
%%%%%\mpla  -> Mod. Phys. Lett.
%%%%%\mplb  -> Mod. Phys. Lett.
%%%%%\nature-> Nature
%%%%%\nim   -> Nucl. Instrum. Meth.
%%%%%\npa   -> Nucl. Phys. A
%%%%%\npb   -> Nucl. Phys. B
%%%%%\npps  -> Nucl. Phys. (Proc. Suppl.)
%%%%%\nc    -> Nuovo Cim.
%%%%%\ncs   -> Nuovo Cim. Suppl.
%%%%%\pan   -> Phys. Atom. Nucl.
%%%%%\pla   -> Phys. Lett. A
%%%%%\plb   -> Phys. Lett. B
%%%%%\pr    -> Phys. Rev.
%%%%%\pra   -> Phys. Rev. A
%%%%%\prb   -> Phys. Rev. B
%%%%%\prc   -> Phys. Rev. C
%%%%%\prd   -> Phys. Rev. D
%%%%%\pre   -> Phys. Rev. E
%%%%%\prep  -> Phys. Rept.
%%%%%\prl   -> Phys. Rev. Lett.
%%%%%\phys  -> Physica
%%%%%\plms  -> Proc. London Math. Soc. B
%%%%%\pnas  -> Proc. Nat. Acad. Sci.
%%%%%\ppnp  -> Prog. Part. Nucl. Phys.
%%%%%\ptp   -> Prog. Theor. Phys.
%%%%%\ptps  -> Prog. Theor. Phys. Suppl.
%%%%%\rmp   -> Rev. Mod. Phys.
%%%%%\sjnp  -> Sov. J. Nucl. Phys.
%%%%%\sjpn  -> Sov. J. Part. Nucl.
%%%%%\jetp  -> Sov. Phys. JETP
%%%%%\jetpl -> Sov. Phys. JETP Lett.
%%%%%\spu   -> Sov. Phys. Usp.
%%%%%\tmf   -> Teor. Mat. Fiz.
%%%%%\tmp   -> Theor. Math. Phys.
%%%%%\ufn   -> Usp. Fiz. Nauk.
%%%%%\ujp   -> Ukr. J. Phys.
%%%%%\yf    -> Yad. Fiz.
%%%%%\zpc   -> Z. Physik C
%%%%%\zetf  -> Zh. Eksp. Teor. Fiz.
%%%%%
%%%%%\ibid  -> ibid.
%%%%%\end{verbatim}
%%%%%\end{multicols}
%%%%%For journals that are not included in this list the command
%%%%%\verb!\newjournal! can be used, that needs five arguments as in the
%%%%%following example:
%%%%%
%%%%%\noindent{\small\verb!\newjournal{J.\ Stat.\ Phys.\ }{JSTPB}{35}{1984}{193} -> !
%%%%%\emph{J.\ Stat.\ Phys.\ }{\bf 35} (1984) 193}
%%%%%
%%%%%\noindent with the link to Slac Spires archive given by the spires-code in the
%%%%%second argument.
%%%%%
%%%%%\paragraph{Archives.}
%%%%%In addition, further shortcuts are provided for the {\tt xxx} archives.
%%%%%They require one argument, that is the combination of year (last two
%%%%%digits), month (two digits) and archive number (three digits);
%%%%%
%%%%%\noindent \verb!\hepth -> {\tt hep-th/#1}!,  and all the others\vspace{-2ex}
%%%%%
%%%%%\begin{verbatim}
%%%%%\hepex, \heplat, \hepph, \accphys, \grqc, \quantph, \nlinsys,
%%%%%\qalg, \alggeom, \solvint, \suprcon, \astroph, \chaodyn, \condmat.
%%%%%\end{verbatim}
%%%%%
%%%%%\noindent and for math archives \verb!\Math{#1}{#2}! where the first argument
%%%%%is for the two capital letters specification of the field and the second is the
%%%%%archive number, e.g.:
%%%%%\begin{verbatim}
%%%%%\Math{QA}{9901241} -> {\tt math.QA/9901241}.
%%%%%\end{verbatim}

%%%%%
%%%%%Notice that the shortcuts above also provide hyperlinks to the online data
%%%%%of the corresponding references. For example:
%%%%%
%%%%%\verb!\cmp{108}{1987}{535}! \ $\rightarrow\ $  \ignorespaces\cmp{108}{1987}{535};
%%%%%
%%%%%\verb!\jhep{07}{1997}{001}! \ $\rightarrow\ $  \ignorespaces\jhep{07}{1997}{001};
%%%%%
%%%%%\verb!\hepth{9604001}     ! \ $\rightarrow\ $  \hepth{9604001}.
%%%%%}
%%%%%
%%%%%
%%%%%
%%%%%\section{Examples}
%%%%%
%%%%%An {\tt eqnarray} to test draft labels and hyper-references.
%%%%%\begin{eqnarray}
%%%%%\sum_{n=-\infty}^\infty x^n &=& \sum_{n=0}^\infty x^{-n} -1
%%%%%                +\sum_{n=0}^\infty x^n\\
%%%%%&= & {1\over1-1/x} -1 +{1\over1-x}=0\,.\label{eq:zero}
%%%%%\end{eqnarray}
%%%%%Of course the radius in eq.~(\ref{eq:zero})\ldots
%%%%%
%%%%%\medskip
%%%%%This is the example for section~\ref{sec:eq}, Euler's (ubiquitous)
%%%%%proof for the existence of God, which contains all basic operations and
%%%%%objects of complex algebra:
%%%%%
%%%%%\begin{equation}
%%%%%{\rm e }^{i\pi} +1 =0\,.
%%%%%\label{eq:pi}
%%%%%\end{equation}
%%%%%
%%%%%
%%%%%
%%%%%\section{About flags and limits}
%%%%%{\small
%%%%%
%%%%%New flags in this class which might be of some interest for advanced
%%%%%users, are \verb!\if@hyper!, \label{sec:flags} \verb!\if@preprint!.
%%%%%They are {\tt true} when processing a {\tt hyper} or
%%%%%a {\tt preprint} version, respectively.
%%%%%\medskip
%%%%%
%%%%%As far as the code for tables and figures is concerned, some critical
%%%%%behavior in the formatting can arise {\it in draft mode}.
%%%%%
%%%%%Especially in conjunction with other floats or when \verb!\FIGURE! or
%%%%%\verb!\TABLE! has a long caption with a label inside. The labels which
%%%%%should be shown on the margin could appear in the wrong order.  The
%%%%%same for citations inside footnotes.  In fact multiple labels inside a
%%%%%float are difficult to show, and could appear superimposed.
%%%%%
%%%%%Other limitations can be found in the documentation of the {\sf floatflt}
%%%%%package \cite{fltf}, and will be hopefully removed in the next release
%%%%%also for the files of this class.
%%%%%
%%%%%}
%%%%%
%%%%%
%%%%%
%%%%%\listoftables       % ONLY IN DRAFT MODE
%%%%%\listoffigures      % ONLY IN DRAFT MODE
%%%%%\begin{thebibliography}{999}
%%%%%\bibitem{proc} F. Nesti and P. Dall'Aglio, \emph{Sample proceedings in
%%%%%        JHEP format}, SISSA 2001.
%%%%%\bibitem{fltf}  Maths Dahlgren, {\it Package {\tt floatflt}, distributed
%%%%%        with \LaTeXe{} 96/06/01}, 1994-1996.
%%%%%\bibitem{LC}    M. Goossens, F. Mittelbach, A. Samarin,
%%%%%                {\it The \LaTeX{} Companion}, Addison-Wesley 1994.
%%%%%\bibitem{TeXbook} D. E. Knuth, {\it The \TeX book}, Addison-Wesley 1986.
%%%%%
%%%%%
%%%%%\end{thebibliography}
%%%%%
%%%%%\end{document}
%%%%%
%%%%%
%%%%%{\footnotesize
%%%%%\begin{verbatim}
%%%%%\adp   -> {\it Adv. Phys. }{\bf #1} (#2) #3
%%%%%\advm  -> {\it Adv. Math. }{\bf #1} (#2) #3
%%%%%\ap    -> {\it Ann. Phys. (NY) }{\bf #1} (#2) #3
%%%%%\apj   -> {\it Astrophys. J. }{\bf #1} (#2) #3
%%%%%\app   -> {\it Astropart. Phys. }{\bf #1} (#2) #3
%%%%%\appol -> {\it Acta Phys. Polon. }{\bf #1} (#2) #3
%%%%%\arnps -> {\it Ann. Rev. Nucl. Part. Sci. }{\bf #1} (#2) #3
%%%%%\atmp  -> {\it Adv. Theor. Math. Phys. }{\bf #1} (#2) #3
%%%%%\bams  -> {\it Bull. Am. Math. Soc. }{\bf #1} (#2) #3
%%%%%\cjm   -> {\it Can. J. Math. }{\bf #1} (#2) #3
%%%%%\cpc   -> {\it Comput. Phys. Commun.}{\bf #1} (#2) #3
%%%%%\cmp   -> {\it Comm. Math. Phys. }{\bf #1} (#2) #3
%%%%%\cqg   -> {\it Class. and Quant. Grav. }{\bf #1} (#2) #3
%%%%%\ctp   -> {\it Comm. Theor. Phys. }{\bf #1} (#2) #3
%%%%%\dmj   -> {\it Duke Math. J. }{\bf #1} (#2) #3
%%%%%\epjc  -> {\it Eur. Phys. J. }{\bf C#1} (#2) #3
%%%%%\epl   -> {\it Europhys. Lett. }{\bf #1} (#2) #3
%%%%%\forp  -> {\it Fortschr. Phys. }{\bf #1} (#2) #3
%%%%%\hpa   -> {\it Helv. Phys. Acta }{\bf #1} (#2) #3
%%%%%\ijmpa -> {\it Int. J. Mod. Phys. }{\bf A #1} (#2) #3
%%%%%\ijmpb -> {\it Int. J. Mod. Phys. }{\bf B #1} (#2) #3
%%%%%\ijtp  -> {\it Int. J. Theor. Phys. }{\bf #1} (#2) #3
%%%%%\invm  -> {\it Invent. Math. }{\bf #1} (#2) #3
%%%%%\jetp  -> {\it Sov. Phys. JETP }{\bf #1} (#2) #3
%%%%%\jetpl -> {\it JETP Lett. }{\bf #1} (#2) #3
%%%%%\jgp   -> {\it J. Geom. Phys. }{\bf #1} (#2) #3
%%%%%\jhep  -> {\it JHEP }{\bf #1} (#2) #3
%%%%%\jmp   -> {\it J. Math. Phys. }{\bf #1} (#2) #3
%%%%%\joth  -> {\it J. Operator Theory }{\bf #1} (#2) #3
%%%%%\jpha  -> {\it J. Phys. }{\bf A#1} (#2) #3
%%%%%\jphg  -> {\it J. Phys. }{\bf G#1} (#2) #3
%%%%%\lmp   -> {\it Lett. Math. Phys. }{\bf #1} (#2) #3
%%%%%\mpla  -> {\it Mod. Phys. Lett. }{\bf A #1} (#2) #3
%%%%%\mplb  -> {\it Mod. Phys. Lett. }{\bf B #1} (#2) #3
%%%%%\nature-> {\it Nature }{\bf #1} (#2) #3
%%%%%\nc    -> {\it Nuovo Cim. }{\bf #1} (#2) #3
%%%%%\ncl   -> {\it Lett. Nuovo Cim. }{\bf #1} (#2) #3
%%%%%\ncs   -> {\it Nuovo Cim. Suppl. }{\bf #1} (#2) #3
%%%%%\nim   -> {\it Nucl. Instrum. Meth. }{\bf #1} (#2) #3
%%%%%\npa   -> {\it Nucl. Phys. }{\bf A #1} (#2) #3
%%%%%\npb   -> {\it Nucl. Phys. }{\bf B #1} (#2) #3
%%%%%\npps  -> {\it Nucl. Phys. }{\bf #1} {\it(Proc. Suppl.)} (#2) #3
%%%%%\phys  -> {\it Physica }{\bf #1} (#2) #3
%%%%%\pla   -> {\it Phys. Lett. }{\bf A #1} (#2) #3
%%%%%\plb   -> {\it Phys. Lett. }{\bf B #1} (#2) #3
%%%%%\pnas  -> {\it Proc. Nat. Acad. Sci. }{\bf #1} (#2) #3
%%%%%\ppnp  -> {\it Prog. Part. Nucl. Phys. }{\bf #1} (#2) #3
%%%%%\pr    -> {\it Phys. Rev. }{\bf #1} (#2) #3
%%%%%\pra   -> {\it Phys. Rev. }{\bf A #1} (#2) #3
%%%%%\prb   -> {\it Phys. Rev. }{\bf B #1} (#2) #3
%%%%%\prc   -> {\it Phys. Rev. }{\bf C #1} (#2) #3
%%%%%\prd   -> {\it Phys. Rev. }{\bf D #1} (#2) #3
%%%%%\pre   -> {\it Phys. Rev. }{\bf E #1} (#2) #3
%%%%%\prep  -> {\it Phys. Rep. }{\bf #1} (#2) #3
%%%%%\prl   -> {\it Phys. Rev. Lett. }{\bf #1} (#2) #3
%%%%%\ptp   -> {\it Prog. Theor. Phys. }{\bf #1} (#2) #3
%%%%%\rmp   -> {\it Rev. Mod. Phys. }{\bf #1} (#2) #3
%%%%%\sjnp  -> {\it Sov. J. Nucl. Phys. }{\bf #1} (#2) #3
%%%%%\yf    -> {\it Yad. Fiz. }{\bf #1} (#2) #3
%%%%%\zetf  -> {\it Zh. Eksp. Teor. Fiz. }{\bf #1} (#2) #3
%%%%%\zpc   -> {\it Z. Physik }{\bf C #1} (#2) #3
%%%%%\ibid  -> {\it ibid. }{\bf #1} (#2) #3
%%%%%\end{verbatim}}

hep-ph0111289.extracted_bib
\begin{thebibliography}{999}
\bibitem{01} D.Fargion: astro-ph/0002453,  Accepted Ap.J.(2001)
\bibitem{02} R. Gandhi, C. Quigg, M.H. Reno, I. Sarcevic: Phys. Rev. D {\bf 58}, 093009 (1998)
\bibitem{03} D. Fargion, A. Aiello, R. Conversano, 26th ICRC, He6.1.09,p.396-398.1999.(USA);
\bibitem{04} D. Fargion,  27th ICRC 2001, HE1.8,Vol-2, Pag. 903-906, 2001.(Germany).
\bibitem{05} X. Bertou et all,astro-ph/0104452.
\bibitem{06} J. G. Learned, S. Pakvasa: Astropart. Phys. {\bf 3}, 267 (1995)
\bibitem{07} D. Fargion, A. Salis, B. Mele: Ap. J. {\bf 517}, 725--733(1999),USA.
% \bibitem{3} J. G. Learned, S. Pakvasa: Astropart. Phys. {\bf 3}, pp. 267 (1995)

%Ref 02%
%\bibitem{02} R. Gandhi, C. Quigg, M.H. Reno, I. Sarcevic: Phys. Rev. D {\bf 58}, 093009 (1998)

%Ref 03%
%\bibitem{11}  D. Fargion, A. Salis: In: {\it Proc. 25th ICRC, Salt Lake City, 1997}, HE-4-6 (1997) pp.~153--156


%\bibitem{16} D. Fargion, A. Salis, B. Mele: Ap. J. {\bf 517}, pp. 725--733 (1999), astro-ph/9710029

%Ref 05%
%\bibitem{17} D. Fargion: Lett. Nuovo Cimento {\bf 31}, 499 (1981)
%\bibitem{17} D. Fargion: Lett. Nuovo Cimento {\bf 31}, pp. 499 (1981)

%Ref 06%
%\bibitem{18} D. Fargion: Nuovo Cimento
%{\bf 65B}, 316 (1981) F. Antonelli, R. Konoplich, D.~Fargion: Lett. Nuovo Cimento {\bf 32}, 289 (1981)

%\bibitem{18} D. Fargion: Nuovo Cimento
%{\bf 65B}, pp. 316 (1981) F. Antonelli, R. Konoplich, D.~Fargion: Lett. Nuovo Cimento {\bf 32}, pp. 289 (1981)


%Ref 07%
%\bibitem{19} D. Fargion: Nuovo Cimento {\bf 77B}, 111 (1983)
% \bibitem{19} D. Fargion: Nuovo Cimento {\bf 77B}, pp. 111 (1983)

%Ref 08%

%Ref 09%
%\bibitem{24} D. Fargion: astro-ph/0002453, (2000); astro-ph/0005439.(2000)

     %Ref 10%
%\bibitem{27} Y.N. Hayashida et al.: In: {\it Proc. 26th ICRC, Salt Lake City, 1999}, OG.1.3.04


%%%%\bibitem{proc} F. Nesti and P. Dall'Aglio, \emph{Sample proceedings in
%%%%        JHEP format}, SISSA 2001.
%%%%\bibitem{fltf}  Maths Dahlgren, {\it Package {\tt floatflt}, distributed
%%%%        with \LaTeXe{} 96/06/01}, 1994-1996.
%%%%\bibitem{LC}    M. Goossens, F. Mittelbach, A. Samarin,
%%%%                {\it The \LaTeX{} Companion}, Addison-Wesley 1994.
%%%%\bibitem{TeXbook} D. E. Knuth, {\it The \TeX book}, Addison-Wesley 1986.


\end{thebibliography}