Elsevier instructions for the preparation of a 2-column format camera-ready paper in \LaTeX
P. de Groot\address[MCSD]{Mathematics and Computer Science Section, Elsevier Science B.V.,
P.O. Box 103, 1000 AC Amsterdam, The Netherlands}% \thanks{Footnotes should appear on the first page only to indicate your present address (if different from your normal address)
research grant
sponsoring agency
etc. These are obtained with the {bs thanks} command.}
R. de Maas\addressmark\thanks{For following authors with the same address use the {bs addressmark} command.}
2 Finch Road, Winchester, Hampshire P3L T19, United Kingdom} and A. Sheffield\addressmark[MCSD]\thanks{To reuse an addressmark later on
label the address with an optional argument to the {bs address} command
e.g. {bs address[MCSD]}
and repeat the label as the optional argument to the {bs addressmark} command
e.g. {bs addressmark[MCSD]}.}
These pages provide you with an example of the layout and style for 100\% reproduction which we wish you to adopt during the preparation of your paper. This is the output from the \LaTeX{} document class you requested. \vspace{1pc}
espcrc2.tex
%%%%%%%%%% espcrc2.tex %%%%%%%%%%
%
% $Id: espcrc2.tex 1.2 2000/07/24 09:12:51 spepping Exp spepping $
%
\documentclass[fleqn,twoside]{article}
\usepackage{espcrc2}

% change this to the following line for use with LaTeX2.09
% \documentstyle[twoside,fleqn,espcrc2]{article}

% if you want to include PostScript figures
\usepackage{graphicx}
% if you have landscape tables
\usepackage[figuresright]{rotating}

% put your own definitions here:
%   \newcommand{\cZ}{\cal{Z}}
%   \newtheorem{def}{Definition}[section]
%   ...
\newcommand{\ttbs}{\char'134}
\newcommand{\AmS}{{\protect\the\textfont2
  A\kern-.1667em\lower.5ex\hbox{M}\kern-.125emS}}

% add words to TeX's hyphenation exception list
\hyphenation{author another created financial paper re-commend-ed Post-Script}

% declarations for front matter
\title{Elsevier instructions for the preparation of a
       2-column format camera-ready paper in \LaTeX}

\author{P. de Groot\address[MCSD]{Mathematics and Computer Science Section, 
        Elsevier Science B.V., \\ 
        P.O. Box 103, 1000 AC Amsterdam, The Netherlands}%
        \thanks{Footnotes should appear on the first page only to
                indicate your present address (if different from your
                normal address), research grant, sponsoring agency, etc.
                These are obtained with the {\tt\ttbs thanks} command.},
        R. de Maas\addressmark\thanks{For following authors with the same
                address use the {\tt\ttbs addressmark} command.},
        X.-Y. Wang\address{Economics Department, University of Winchester, \\
        2 Finch Road, Winchester, Hampshire P3L T19, United Kingdom}
        and
        A. Sheffield\addressmark[MCSD]\thanks{To reuse an addressmark
                later on, label the address with an optional argument to the
                {\tt \ttbs address} command, e.g. {\tt\ttbs
                address[MCSD]}, and repeat the label
                as the optional argument to the {\tt\ttbs addressmark}
                command, e.g. {\tt\ttbs addressmark[MCSD]}.}}
       
\begin{document}

\begin{abstract}
These pages provide you with an example of the layout and style for
100\% reproduction which we wish you to adopt during the preparation of
your paper. This is the output from the \LaTeX{} document class you
requested.
\vspace{1pc}
\end{abstract}

% typeset front matter (including abstract)
\maketitle

\section{FORMAT}

Text should be produced within the dimensions shown on these pages:
each column 7.5 cm wide with 1 cm middle margin, total width of 16 cm
and a maximum length of 19.5 cm on first pages and 21 cm on second and
following pages. The \LaTeX{} document class uses the maximum stipulated
length apart from the following two exceptions (i) \LaTeX{} does not
begin a new section directly at the bottom of a page, but transfers the
heading to the top of the next page; (ii) \LaTeX{} never (well, hardly
ever) exceeds the length of the text area in order to complete a
section of text or a paragraph. Here are some references:
\cite{Scho70,Mazu84}.

\subsection{Spacing}

We normally recommend the use of 1.0 (single) line spacing. However,
when typing complicated mathematical text \LaTeX{} automatically
increases the space between text lines in order to prevent sub- and
superscript fonts overlapping one another and making your printed
matter illegible.

\subsection{Fonts}

These instructions have been produced using a 10 point Computer Modern
Roman. Other recommended fonts are 10 point Times Roman, New Century
Schoolbook, Bookman Light and Palatino.

\section{PRINTOUT}

The most suitable printer is a laser or an inkjet printer. A dot
matrix printer should only be used if it possesses an 18 or 24 pin
printhead (``letter-quality'').

The printout submitted should be an original; a photocopy is not
acceptable. Please make use of good quality plain white A4 (or US
Letter) paper size. {\em The dimensions shown here should be strictly
adhered to: do not make changes to these dimensions, which are
determined by the document class}. The document class leaves at least
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number.

Printers sometimes produce text which contains light and dark streaks,
or has considerable lighting variation either between left-hand and
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optimal reproduction quality, the contrast of text lettering must be
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If corrections are made to the text, print completely new replacement
pages. The contrast on these pages should be consistent with the rest
of the paper as should text dimensions and font sizes.

\section{TABLES AND ILLUSTRATIONS}

Tables should be made with \LaTeX; illustrations should be originals or
sharp prints. They should be arranged throughout the text and
preferably be included {\em on the same page as they are first
discussed}. They should have a self-contained caption and be positioned
in flush-left alignment with the text margin within the column. If they
do not fit into one column they may be placed across both columns
(using \verb-\begin{table*}- or \verb-\begin{figure*}- so that they
appear at the top of a page).

\subsection{Tables}

Tables should be presented in the form shown in
Table~\ref{table:1}.  Their layout should be consistent
throughout.

\begin{table*}[htb]
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:1}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\tabcolsep}{2pc} % enlarge column spacing
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular}{@{}lllll}
\hline
$\Lambda$ (MeV)           & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} \\
\hline
$r_d$ (fm)                & \m1.973 & \m1.972 & \m1.974 & \m1.978 \\
$Q_d$ ($\mbox{fm}^2$)     & \m0.259 & \m0.268 & \m0.287 & \m0.302 \\
$P_D$ (\%)                & \m2.32  & \m2.83  & \m4.34  & \m6.14  \\
$\mu_d$                   & \m0.867 & \m0.864 & \m0.855 & \m0.845 \\
$\mathcal{M}_{\mathrm{M1}}$ (fm)   & \m3.995 & \m3.989 & \m3.973 & \m3.955 \\
$\mathcal{M}_{\mathrm{GT}}$ (fm)   & \m4.887 & \m4.881 & \m4.864 & \m4.846 \\
$\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   
                          & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) 
                          & \m0.03  & \m0.03  & \m0.03  & \m0.03  \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) 
                          & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ \\
\hline
\end{tabular}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{table*}

\begin{sidewaystable}
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:2}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular*}{\textheight}{@{\extracolsep{\fill}}lllllllllllll}
\hline
& $\Lambda$ (MeV) & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} & \cc{$225$} & \cc{$250$} &
\cc{Exp.} & \cc{$v_{18}$~\cite{v18}} &  \\
\hline
%b
 & $r_d$ (fm)                        & \m1.973 & \m1.972 & \m1.974 & \m1.978 & \m1.983 & \m1.987 & 1.966(7) & \m1.967 & \\[2pt]
 & $Q_d$ ($\mbox{fm}^2$)             & \m0.259 & \m0.268 & \m0.287 & \m0.302 & \m0.312 & \m0.319 & 0.286    & \m0.270 & \\[2pt]
 & $P_D$ (\%)                        & \m2.32  & \m2.83  & \m4.34  & \m6.14  & \m8.09  & \m9.90  & $-$      & \m5.76  & \\[2pt]
 & $\mu_d$                           & \m0.867 & \m0.864 & \m0.855 & \m0.845 & \m0.834 & \m0.823 & 0.8574   & \m0.847 & \\[5pt]
 & $\mathcal{M}_{\mathrm{M1}}$ (fm)             & \m3.995 & \m3.989 & \m3.973 & \m3.955 & \m3.936 & \m3.918 & $-$      & \m3.979 & \\[5pt]
 & $\mathcal{M}_{\mathrm{GT}}$ (fm)             & \m4.887 & \m4.881 & \m4.864 & \m4.846 & \m4.827 & \m4.810 & $-$      & \m4.859 & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.44$ & $-$      & $-0.45$ & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & $-$      & \m0.03  & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ & $-0.12$ & $-0.10$ & $-$      & $-0.21$ & \\
\hline
\end{tabular*}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{sidewaystable}

Horizontal lines should be placed above and below table headings, above
the subheadings and at the end of the table above any notes. Vertical
lines should be avoided.

If a table is too long to fit onto one page, the table number and
headings should be repeated above the continuation of the table. For
this you have to reset the table counter with
\verb|\addtocounter{table}{-1}|. Alternatively, the table can be turned
by $90^\circ$ (`landscape mode') and spread over two consecutive pages
(first an even-numbered, then an odd-numbered one) created by means of
\verb|\begin{table}[h]| without a caption. To do this, you prepare the
table as a separate \LaTeX{} document and attach the tables to the
empty pages with a few spots of suitable glue.

\subsection{Useful table packages}

Modern \LaTeX{} comes with several packages for tables that
provide additional functionality. Below we mention a few. See
the documentation of the individual packages for more details. The
packages can be found in \LaTeX's \texttt{tools} directory.

\begin{description}
  
\item[\texttt{array}] Various extensions to \LaTeX's \texttt{array}
  and \texttt{tabular} environments.
  
\item[\texttt{longtable}] Automatically break tables over several
  pages. Put the table in the \texttt{longtable} environment instead
  of the \texttt{table} environment.
  
\item [\texttt{dcolumn}] Define your own type of column. Among others,
  this is one way to obtain alignment on the decimal point.

\item[\texttt{tabularx}] Smart column width calculation within a
  specified table width.
  
\item[\texttt{rotating}] Print a page with a wide table or figure in
  landscape orientation using the \texttt{sidewaystable} or
  \texttt{sidewaysfigure} environments, and many other rotating
  tricks. Use the package with the \texttt{figuresright} option to
  make all tables and figures rotate in clockwise. Use the starred
  form of the \texttt{sideways} environments to obtain full-width
  tables or figures in a two-column article.

\end{description}

\subsection{Line drawings}

Line drawings may consist of laser-printed graphics or professionally
drawn figures attached to the manuscript page. All figures should be
clearly displayed by leaving at least one line of spacing above and
below them. When placing a figure at the top of a page, the top of the
figure should align with the bottom of the first text line of the other
column.

Do not use too light or too dark shading in your figures; too dark a
shading may become too dense while a very light shading made of tiny
points may fade away during reproduction.

All notations and lettering should be no less than 2\,mm high. The use
of heavy black, bold lettering should be avoided as this will look
unpleasantly dark when printed.

\subsection{PostScript figures}

Instead of providing separate drawings or prints of the figures you
may also use PostScript files which are included into your \LaTeX{}
file and printed together with the text. Use one of the packages from
\LaTeX's \texttt{graphics} directory: \texttt{graphics},
\texttt{graphicx} or \texttt{epsfig}, with the \verb|\usepackage|
command, and then use the appropriate commands
(\verb|\includegraphics| or \verb|\epsfig|) to include your PostScript
file.

The simplest command is: \newline
\verb|\includegraphics{file}|, which inserts the
PostScript file \texttt{file} at its own size. The starred version of
this command: \newline
\verb|\includegraphics*{file}|, does the same, but clips
the figure to its bounding box.

With the \texttt{graphicx} package one may specify a series of options
as a key--value list, e.g.:
\begin{tabular}{@{}l}
\verb|\includegraphics[width=15pc]{file}|\\
\verb|\includegraphics[height=5pc]{file}|\\
\verb|\includegraphics[scale=0.6]{file}|\\
\verb|\includegraphics[angle=90,width=20pc]{file}|
\end{tabular}

See the file \texttt{grfguide}, section ``Including Graphics Files'',
of the \texttt{graphics} distribution for all options and a detailed
description.

The \texttt{epsfig} package mimicks the commands familiar from the
package with the same name in \LaTeX2.09. A PostScript file
\texttt{file} is included with the command
\verb|\psfig{file=file}|.

Grey-scale and colour photographs cannot be included in this way,
since reproduction from the printed CRC article would give
insufficient typographical quality. See the following subsections.

\begin{figure}[htb]
\vspace{9pt}
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Good sharp prints should be used and not (distorted) photocopies.}
\label{fig:largenenough}
\end{figure}
%
\begin{figure}[htb]
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Remember to keep details clear and large enough.}
\label{fig:toosmall}
\end{figure}

\subsection{Black and white photographs}

Photographs must always be sharp originals ({\em not screened
versions\/}) and rich in contrast. They will undergo the same reduction
as the text and should be pasted on your page in the same way as line
drawings.

\subsection{Colour photographs}

Sharp originals ({\em not transparencies or slides\/}) should be
submitted close to the size expected in publication. Charges for the
processing and printing of colour will be passed on to the author(s) of
the paper. As costs involved are per page, care should be taken in the
selection of size and shape so that two or more illustrations may be
fitted together on one page. Please contact the Author Support
Department at Elsevier (E-mail: \texttt{authorsupport@elsevier.nl})
for a price quotation and layout instructions before producing your
paper in its final form.

\section{EQUATIONS}

Equations should be flush-left with the text margin; \LaTeX{} ensures
that the equation is preceded and followed by one line of white space.
\LaTeX{} provides the document class option {\tt fleqn} to get the
flush-left effect.

\begin{equation}
H_{\alpha\beta}(\omega) = E_\alpha^{(0)}(\omega) \delta_{\alpha\beta} +
                          \langle \alpha | W_\pi | \beta \rangle 
\end{equation}

You need not put in equation numbers, since this is taken care of
automatically. The equation numbers are always consecutive and are
printed in parentheses flush with the right-hand margin of the text and
level with the last line of the equation. For multi-line equations, use
the {\tt eqnarray} environment.

For complex mathematics, use the \AmS math package. This package
sets the math indentation to a positive value. To keep the equations
flush left, either load the \texttt{espcrc} package \emph{after} the
\AmS math package or set the command \verb|\mathindent=0pt| in the
preamble of your article.

\begin{thebibliography}{9}
\bibitem{Scho70} S. Scholes, Discuss. Faraday Soc. No. 50 (1970) 222.
\bibitem{Mazu84} O.V. Mazurin and E.A. Porai-Koshits (eds.),
                 Phase Separation in Glass, North-Holland, Amsterdam, 1984.
\bibitem{Dimi75} Y. Dimitriev and E. Kashchieva, 
                 J. Mater. Sci. 10 (1975) 1419.
\bibitem{Eato75} D.L. Eaton, Porous Glass Support Material,
                 US Patent No. 3 904 422 (1975).
\end{thebibliography}

References should be collected at the end of your paper. Do not begin
them on a new page unless this is absolutely necessary. They should be
prepared according to the sequential numeric system making sure that
all material mentioned is generally available to the reader. Use
\verb+\cite+ to refer to the entries in the bibliography so that your
accumulated list corresponds to the citations made in the text body. 

Above we have listed some references according to the
sequential numeric system \cite{Scho70,Mazu84,Dimi75,Eato75}.
\end{document}

paper.tex
%%%%%%%%%% espcrc2.tex %%%%%%%%%%
%
% $Id: espcrc2.tex 1.2 2000/07/24 09:12:51 spepping Exp spepping $
%
\documentclass[fleqn,twoside]{article}
\usepackage{espcrc2}

% change this to the following line for use with LaTeX2.09
% \documentstyle[twoside,fleqn,espcrc2]{article}

% if you want to include PostScript figures
\usepackage{graphicx}
% if you have landscape tables
\usepackage[figuresright]{rotating}

% put your own definitions here:
%   \newcommand{\cZ}{\cal{Z}}
%   \newtheorem{def}{Definition}[section]
%   ...
\newcommand{\ttbs}{\char'134}
\newcommand{\AmS}{{\protect\the\textfont2
  A\kern-.1667em\lower.5ex\hbox{M}\kern-.125emS}}

% add words to TeX's hyphenation exception list
\hyphenation{author another created financial paper re-commend-ed Post-Script}

\begin{document}


% declarations for front matter
\title{Centauros and/or Chirons as evaporating mini black holes}

\author{Theodore N. Tomaras\address{Department of Physics and Institute of
Plasma Physics, University of Crete, \\
P.O.Box 2208, 71003 Heraklion, Crete, Hellas \\ 
and Fo.R.T.H.} 
        \thanks{This talk is mostly based on \cite{mmt}. 
	Research supported in part by the EU under the RTN contract
	HPRN-CT-2000-00122, and by a grant P.O. Education - Heraklitos
	from the Hellenic Ministry of Education.}}
       
%\begin{document}

\begin{abstract}
It is argued that the signals expected from the evaporation of mini 
black holes - predicted in TeV-scale gravity models with large extra 
dimensions, and possibly produced in ultra high energy collisions in the
atmosphere - have characteristics quite similar to the ones of the Centauro
events, an old mystery of cosmic-ray physics.

\vspace{1pc}
\end{abstract}

% typeset front matter (including abstract)
\maketitle

\section{Introduction}

The theoretical framework of this talk is the {\it TeV-scale gravity
with large extra dimensions}. The basic assumption, easily accomodated in 
Superstring Theory, is that our spacetime is a 4 dimensional hypersurface
(a {\it D3-brane}) embedded in a 10 dimensional world (the {\it bulk}), 
with the additional feature
that all known matter (quarks, leptons, higgses), as well as the carriers of
the fundamental interactions of the Standard Model of Particle Physics 
(photon, W, Z, gluons) are
confined on our 4 dimensional subspace. Only gravity can propagate in
the bulk. The fact that the only communication with the bulk is via the 
gravitational force, allows for a fundamental gravitational scale to be
of ${\cal O}$(1TeV), while at the same time the size of the extra spatial
dimensions may be as large as a fraction of a mm. 

Clearly, such a scenario, if true, leads to the exciting prospect of 
observing string physics, large higher dimensions and quantum gravity effects, 
within the next few years in the forthcoming accelerator (LHC), neutrino and 
cosmic-ray experiments.

Even better, in this talk I will argue that the long known Centauro-like 
events (CLEs) may be due to the formation and subsequent evaporation of 
mini black holes
(MBHs), predicted in the context of the above scenario \cite{mmt}. 
After a quick review of the relevant scales and of the main features of 
MBHs in TeV-gravity, as well as of the basic characteristics of the 
Centauro events, I present in Section 5 the somewhat qualitative arguments
that support our interpretation. The talk ends with a critical discussion.

The first steps towards a more quantitative analytical/Monte Carlo 
investigation of the mini black 
hole picture are described in \cite{cct} and \cite{cct2}.




\section{TeV-scale gravity models}

Even though non-compact extra dimensions are not a priori excluded,
the most straightforward realization of the above theoretical scenario 
is to neglect the
tension on the brane, which would modify the gravitational background, 
and to consider
the extra dimensions compact and forming a higher dimensional torus $T^n$, 
with equal radii $R$.  
 
In the simplest case of $n=1$, one is dealing with a 4 dimensional Minkowski
space with one extra transverse dimension, a circle of radius $R$. 
One may compute the gravitational potential $\Phi({{\bf x},\theta})$
(in the Newtonian approximation) of a point mass $M$ at the origin, by solving
the corresponding Poisson equation
\begin{equation}
\nabla^2 \Phi+{1\over R^2}\frac{\partial^2\Phi}{\partial\theta^2}=
-G^{(4)}M\delta({\bf x})\frac{\delta(\theta)}{2\pi R}
\label{poisson}
\end{equation}
where $G^{(4)}\equiv 1/M_*^3$ is the 4 dimensional gravitational constant,
with fundamental gravitational scale equal to $M_*$.
Its solution is 
\begin{equation}
\Phi({\bf x},\theta)=\frac{2\pi M G^{(4)}}{Rr}
\frac{1-e^{-2r/R}}{1-2e^{-r/R}\cos\theta+e^{-2r/R}}
\label{potential}
\end{equation}
where $r=|{\bf x}|$ and $\theta$ is the position in the compact
transverse direction. 
Near the mass $M$, i.e. for $r\ll R$ and $\theta\ll\pi$ it gives 
$\Phi\sim 4\pi MG^{(4)}/(r^2+R^2\theta^2)$, the correct expression for a 
4 dimensional gravitational potential. At large distances ($r\gg R$) 
from the mass $M$, on the other hand, one obtains 
$\Phi\sim 2\pi M G^{(4)}/Rr$, the correct 3 dimensional Newtonian 
potential with Newton's constant $G_N=2\pi G^{(4)}/R=2\pi/RM_*^3$. 

These formulas generalize trivially to n toroidal 
transverse dimensions, in which case
Newton's constant is given by
\begin{equation}
G_N\sim {1\over {M_*^2}}{1\over{(RM_*)^n}}
\label{GN}
\end{equation}

{\it Assume} that the fundamental scale $M_*$ of gravity is of the order of the weak 
interaction scale $M_*\sim {\cal O}$(1TeV). Then, (\ref{GN}) leads to the 
correct value $G_N\simeq 10^{-38}$GeV$^{-2}$ for a value of R given by
$R_n\simeq 1/(M_*(M_*^2 G_N)^{1/n})$. 
The value $n=1$ is excluded, since it leads to R of the order of the size 
of the solar system. For $n=2$ one obtains $R_2\sim 2$mm. 
Accelerator and astrophysical constraints lead to a prefered value of $n\geq 4$
with a corresponding value for R, much larger than the usual value $10^{-33}$cm. 



\section{Mini black holes}

As described, the world contains black holes, generalizations to $D=4+n$
spacetime dimensions of the well known Schwarzschild metric.
They are characterized by their mass $M_{BH}$, and can exist as long as
$M_{BH}$ is at least a few times the fundamental gravity scale. Lighter black holes 
cannot exist. Thus, it is reasonable to expect that for $M_*$ a fraction of a TeV, 
the black hole masses are $M_{BH}\geq 2$TeV. 
If, in addition, 
$M_{BH}\ll M_* (G_N M_*^2)^{-(n+1)/n}$, the black hole is essentially 4+n-dimensional,
since its Schwarzschild radius $R_S^{-1}\sim M_* (M_*/M_{BH})^{(1/n+1)}\sim M_*$ 
is much smaller than the radius of the large extra dimensions.
Black holes are expected to be produced in the collision of any two particles, as long
as their impact parameter is smaller than the Schwarzschild radius corresponding
to their center of mass energy. A black hole with mass of the order of the ones
discussed here can be produced in the collision of an ultra high energy primary with
atmospheric partons. The energy of the primary should exceed 1000 TeV and the 
cross section of the process is conjectured to be $\sigma\sim \pi R_S^2 \sim 10^{-37}cm^2
\sim \sigma_{\nu N}^{weak}$, comparable to the neutrino-nucleon
weak interaction cross section at these energies.  

Once produced, black holes are believed to evaporate. 
Even though noone has worked out the details of the evaporation process for such
light black holes, we shall assume the semiclassical formulas of the standard 
treatment. So, within $\tau_{BH}\sim M_*^{n+2} (4\pi R_S)^{n+3}/(n+1)^{n+3}\sim
10^{-27}$seconds the black hole decays "democratically" into all kinds of 
quarks, leptons, gauge bosons, gravitons, higgses. It is a fireball of temperature
$T_{BH}=(n+1)/4\pi R_S\sim 1$TeV. The number of initial particles emitted
by the black hole is determined by its entropy $N_{\rm initial}
\sim S_{BH}=\pi M_{BH}R_S/2$. For the case of black holes with mass of order 1-2 TeV 
of interest here and $n=4$, this number is of the order of ${\cal O}$(10).



\section{The Centauro-like events (CLEs)}

A normal high energy cosmic ray event is created by the collision of a primary
particle with a particle in the atmosphere. Typically a couple of leading partons
emerge from the interaction region with high transverse momenta, leaving
behind a number of soft fragments, mainly pions with relative abundance 1:1:1. 
The neutral pions subsequently decay to photons and the shower ends up
consisting of low $p_T<1$ GeV/c particles with $N_{\rm hadron}/N_{\rm em}\sim 1$ 
or even less, if one takes into account the extra photons that will be produced
as the shower develops even further.

In contrast to the above picture, several events have been observed since 1972
with the following main characteristics \cite{ewa}:
(a) They were claimed to have taken place at distances smaller that 500 m 
above the detectors at Pamir and Chacaltaya. It should be pointed out, however, 
that the altitude was measured directly only for one of these events, and even that
has been questioned recently \cite{OST}. (b) They are hadron rich, with typically
$N_{\rm hadron}/N_{\rm em}\gg 1$, (c) have fragments with high $p_T\gg 1$ GeV/c,
(d) have in many cases a heavy central core with tiny angular opening (halo) and finally, 
(e) have all been observed with energies above a threshold around 
500 TeV in the lab frame.

It should be pointed out that there are severe uncertainties in the observational
data. One of the speakers in this meeting presented a reanalysis of the Centauro I 
and raised serious doubts about the altitudes reported in general 
for all these events \cite{OST}. Others express doubts about the existence of these
events altogether, worrying, for instance, 
about the fact that no such events have been observed
yet in Kanbala and Fuji. We shall not take part in this debate at this point. 
Instead, we shall assume that the events are real and try to interpret them 
as due to evaporating MBHs, produced by ultra high energy 
$E_1>1000$TeV cosmic ray primaries.



\section{CLEs as evaporating mini black holes}

The processes of black hole creation, of its subsequent  evaporation and, finally
of the shower formation in the atmosphere involve all the complications
of several different fields, such as cosmic ray physics, quantum gravity/string theory,
quantum field theory in curved spacetimes,
quark-gluon plasma physics in QCD, low energy non-perturbative QCD,
cosmic shower atmospheric physics, of theoretical and experimental high energy
physics and astrophysics. Given the incomplete knowledge in all these,
a lot has to be done before one can safely confront the observational data.
Nevertheless, we shall make a few simplifying assumptions, implicit in the 
discussion below, and present the arguments 
in favour of the scenario proposed in \cite{mmt,cct,cct2}.

$\bullet$ {\it Energy threshold}. The energy threshold of the observed Centauro
events, corresponds in the center of mass frame to a mass roughly a few times 
$M_*\sim 1$TeV. This coincides with the lower bound on the MBH masses,
mentioned above. The agreement may be even better, if one takes into account 
the energy losses into the bulk 
during the evaporation of the MBH. 

$\bullet$ {\it Production rate}. Assuming that the black holes are produced by
primary neutrinos, one may obtain a rough estimate of the number of
CLEs based on current figures for the neutrino flux $\Phi_\nu$. 
Since we are interested in neutrino energies of order $10^6-10^7$GeV in the lab frame,
one may use the estimates for the gamma-ray burst muon neutrino flux given in
\cite{wb,w}. Their analysis leads to $\sim$20 neutrino-induced muon events in a 
km$^3$ water or ice per year. Since the cross section of MBH production
by neutrinos is of the same order of magnitude as that of muon production, we would
expect approximately the above number of black holes for each kind of neutrino. 
Multiplying by 10-20 (the number of initial jets) and taking into account the 
lower density of the atmosphere, where the centauros are produced, one ends up
with the estimate of about 10-100 events per km$^2$ per year, which is one to two 
orders of magnitude smaller than the claimed intensity of the Centauros \cite{ewa}. 
However, it seems to us that there is considerable uncertainty in the neutrino 
flux, which could take care of this discrepancy \cite{kalashev}.

$\bullet$ {\it Decay products}, $p_T , N_{\rm hadron}/N_{\rm em}$. The black hole, 
depending on its mass, decays initially to 10-20 fundamental particles of all 
kinds and with equal probability. Their energies are $\sim$100 GeV each in the 
black hole frame. The MBH emits almost as a black body of temperature 
$\sim$1 TeV, all types of matter and force quanta of the Standard Model.
The simplest possibility is that these initial partons, with $p_T$s also around
50-100 GeV will form hadrons, mostly mesons, of all kinds.  
The charmed or heavier mesons will decay to lighter ones, the neutral pions will 
decay to photons almost immediately, but the kaons will 
survive a distance of a few hundred meters. Since the Ks are counted as hadrons,
the ratio of $N_{\rm hadron}/N_{\rm em}$ will be enhanced, if the observation takes 
place at less than a few hundred meters from the initial interaction. 
The total multiplicities of the final showers in this case are a few decades \cite{cct}.

An alternative possibility is that a hot DCC forms before hadronization of the 
produced partons. This is known to lead to larger numbers of heavier mesons, which
makes it more probable to obtain a large ratio of the hadronic to the 
electromagnetic components. However, it is unclear if the system passes through 
such a DCC state. In any case, it seems that the probability to obtain a superclean 
Centauro event is rather small.

On the other hand, given the typically large values of $p_T$, 
the present scenario seems to be the most natural one to explain
this feature of the Centauros \cite{ewa2}. 


$\bullet$ {\it Deep penetration}. The deep penetration follows from the assumption
of neutrinos, or some other weakly interacting particle (WIMP?), as the primary 
source of these events. According to the present picture any black holes produced
at higher altitudes from the detectors, will give signals similar to standard 
events \cite{cct}.  This kind of signature with large hadronic to electromagnetic
ratio, could only be obtained from the decay of black holes near the detector.


$\bullet$ {\it Halo}. At a more speculative level, it has been claimed 
recently \cite{cir} that after evaporation
a MBH is expected to leave behind a highly excited string state 
(a string ball), which in principle will decay to light (compared to $M_*$)
particles. Their life-time depends strongly on the excitation level and can be
considerably larger than $M_*^{-1}$. These objects may be serious candidates
in the context of the present scenario for the projectiles responsible for
the halos observed mostly in Chirons.



\section{Discussion}

On the basis of the above qualitative presentation and of the results
of the first numerical
steps taken in \cite{cct,cct2}, it seems that the above scenario may account
quite succesfully (a) for the energy threshold of all these events 
of order ${\cal O}$(TeV) in the center of mass frame, (b) the total multiplicities 
of a few dozen particles, dependent on the number of extra dimensions \cite{cct}, 
(c) the large values of $p_T$, and (d) the number and the rough heights of first 
interaction of the Centauro/Chiron events. It seems less succesfull in giving the right
$N_{\rm hadron}/N_{\rm em}$ (especially for the superclean events), even though
due to large statistical fluctuations, the numerical simulations \cite{cct} have not
been conclusive yet.  

Several alternative proposals have been put forward to explain these mysterious
events \cite{ewa}. An effort was made in \cite{mmt} and \cite{ewa2} to compare the 
various scenaria.
It should be clear however, that the study, for instance, of the production and 
evaporation processes of a MBH or of Strange Quark Matter 
fireballs, of the potential formation of a
high temperature quark-gluon plasma phase or of a DCC, of the hadronization of the 
100 GeV partons, all rely on unknown aspects of the physics involved.
Much more work is necessary and all possible realizations of a given scenario 
have to be investigated, before one can safely 
fit the observational data. The fundamental importance of the issues involved 
deserves every effort.



\begin{thebibliography}{9}

\bibitem{mmt} "Can Centauros or Chirons be the first observations of
evaporating mini black holes?", A.Mironov, A.Morozov and T.N.Tomaras;
hep-ph/0311318.
\bibitem{cct} A.Cafarella, C.Corian\`o and T.N.Tomaras, ``Cosmic Ray Signals
from Mini Black Holes in models with Extra Dimensions: An Analytical/Monte Carlo
study'', hep-ph/0410358.
\bibitem{cct2} A.Cafarella, C.Corian\`o and T.N.Tomaras, ``Searching for Extra
Dimensions in High Energy Cosmic Rays'', hep-ph/0410190. Talk presented in this
meeting by Claudio Corian\`o.
\bibitem{ewa} E.Gladysz-Dziadu\'s, Phys. Part. Nucl. {\bf 34} (2003) 565; 
hep-ph/0111163, and references therein.
\bibitem{OST} V.Kopenkin, A.Ohsawa, E.Shibuya and M.Tamada, Proc. 28th International
Cosmic Ray Conf., 2003; p.1583. V.Kopenkin, Y.Fujimoto and T.Sinzi, Phys. Rev.
{\bf D68} (2003) 052007.
\bibitem{wb} E.Waxman and J.N.Bahcall, Phys. Rev. {\bf D59} (1999) 023002;
hep-ph/9902383.
\bibitem{w} E.Waxman, Nucl. Phys. Proc. Suppl. {\bf 118} (2003) 353.
\bibitem{kalashev} O.E.Kalashev, V.A.Kuzmin, D.V.Semikoz and G.Sigl,
Phys. Rev. {\bf D66} (2002) 063004.
\bibitem{ewa2} E.Gladysz-Dziadu\'s, hep-ph/0405115.
\bibitem{cir} D.Chialva, R.Iengo and J.Russo, hep-th/0310283.

\end{thebibliography}


\end{document}

\section{PRINTOUT}

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\section{TABLES AND ILLUSTRATIONS}

Tables should be made with \LaTeX; illustrations should be originals or
sharp prints. They should be arranged throughout the text and
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appear at the top of a page).



\subsection{Tables}

Tables should be presented in the form shown in
Table~\ref{table:1}.  Their layout should be consistent
throughout.



\vfill

\eject

\newpage




\begin{sidewaystable}

%\underline {Table}
%\footnote{In the Table, we marked with boldface the entries that
%are in {\bf good} agreement with the CLEs, while \underline{disagreeing} items are
%underlined. Minuses also imply \underline{disagreement}.}
%{\small{
%\rotate{
%\verb
\caption{Table}

\begin{tabular}{|c|c|c|c|c|c|c|c|c|c|c|c|}
\hline
&Number of free&Deep&Threshold&$N_{CLE}/N_{total}$&Mass of&Temp.&
Life/decay&Multiplicity&$N_{\gamma}/N_h$&$p_T$-distribution&Halo
\\
&parameters&pen.\footnote{}&Energy\footnote{}&\footnote{}&
the IS\footnote{}&of the IS&time of the IS\footnote{}&of hadrons&&&&
\\
\hline
Usual&&-&No&&&&&$\sim 35$&$\sim 2$&0.4-0.8 GeV/c&\\
events\footnote{}&&&&&&&&&&&-\\
\hline
Centauros&&+&1.8 (6.9) TeV\footnote{}&2.5\%\footnote{}&&&&60-90&low\footnote{}&
1.7 GeV/c&\\
\hline
Mini&&+&1.3 TeV&5\%\footnote{}\addtocounter{footnote}{-2}
&&&&10-20&low\footnote{}&\addtocounter{footnote}1
1.7 GeV/c&\\
Centauros&&&&&&&&&&&\\
\hline
Chirons&&+&1.8 TeV&7\%\footnote{}&&
\addtocounter{footnote}{-3}&&10-20&low\footnote{}&
\addtocounter{footnote}{2} 10-15 GeV/c&+\\
\hline
\hline
MBH&{\bf few}: $M_{BH}$, $M_P$\footnote{}
&{\bf +}&$M_{BH}>M_P$&\underline{$\sim 0.0001\%$}\footnote{}&$M_{BH}$&$\sim M_P$&
$10^{-27}$ s&
$N_{in}={M_{BH}\over 2M_P}$&{\bf low}&{\bf very wide}&{\bf +}\\
&&&&{\bf few \% ?}\footnote{}&&&\footnote{}&
$N_{obs}=?$\footnote{}&&{\bf and flatten}\footnote{}&\\
\hline
\hline
Fireballs&model-dependent
&-&$2\pm 0.5$ TeV&&180 GeV&$T_{QGP}$&$10^{-23}$-$10^{-24}$ s&{\bf 15 to
100}\footnote{}&\underline{$\sim 2$}&{\bf wide}&-\\
\hline
QGP/DCC& DCC direction
&-&$E\gg T_{QGP}$\footnote{}&&&$>$150 MeV&$10^{-23}$-$10^{-24}$ s&&
{\bf low}\footnote{}&\underline{narrow}\footnote{}&-\\
\hline
Strangelets&$s$-quark density&{\bf +}&&&&&&&{\bf low}\footnote{}&&\\
&baryon number&&&&&&&&&&\\
\cite{stfire}&\underline{many}
&{\bf +}&$2\pm 0.5$ TeV&&180 GeV&130 MeV&$10^{-23}$-$10^{-24}$ s \footnote{}
&{\bf 75}&{\bf low}&{\bf wide}&{\bf +}\\
\cite{wilk}&\underline{many}&{\bf +}&300-400 GeV&Depends&300-400&&&&{\bf low}&
\underline{narrow}&{\bf +}\\
&&&&on flux&GeV&&&&&&\\
\hline
\end{tabular}

\end{sidewaystable}


\begin{table*}[htb]
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:1}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\tabcolsep}{2pc} % enlarge column spacing
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular}{@{}lllll}
\hline
$\Lambda$ (MeV)           & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} \\
\hline
$r_d$ (fm)                & \m1.973 & \m1.972 & \m1.974 & \m1.978 \\
$Q_d$ ($\mbox{fm}^2$)     & \m0.259 & \m0.268 & \m0.287 & \m0.302 \\
$P_D$ (\%)                & \m2.32  & \m2.83  & \m4.34  & \m6.14  \\
$\mu_d$                   & \m0.867 & \m0.864 & \m0.855 & \m0.845 \\
$\mathcal{M}_{\mathrm{M1}}$ (fm)   & \m3.995 & \m3.989 & \m3.973 & \m3.955 \\
$\mathcal{M}_{\mathrm{GT}}$ (fm)   & \m4.887 & \m4.881 & \m4.864 & \m4.846 \\
$\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   
                          & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) 
                          & \m0.03  & \m0.03  & \m0.03  & \m0.03  \\
$\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) 
                          & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ \\
\hline
\end{tabular}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{table*}

\begin{sidewaystable}
\caption{The next-to-leading order (NLO) results
{\em without} the pion field.}
\label{table:2}
\newcommand{\m}{\hphantom{$-$}}
\newcommand{\cc}[1]{\multicolumn{1}{c}{#1}}
\renewcommand{\arraystretch}{1.2} % enlarge line spacing
\begin{tabular*}{\textheight}{@{\extracolsep{\fill}}lllllllllllll}
\hline
& $\Lambda$ (MeV) & \cc{$140$} & \cc{$150$} & \cc{$175$} & \cc{$200$} & \cc{$225$} & \cc{$250$} &
\cc{Exp.} & \cc{$v_{18}$~\cite{v18}} &  \\
\hline
%b
 & $r_d$ (fm)                        & \m1.973 & \m1.972 & \m1.974 & \m1.978 & \m1.983 & \m1.987 & 1.966(7) & \m1.967 & \\[2pt]
 & $Q_d$ ($\mbox{fm}^2$)             & \m0.259 & \m0.268 & \m0.287 & \m0.302 & \m0.312 & \m0.319 & 0.286    & \m0.270 & \\[2pt]
 & $P_D$ (\%)                        & \m2.32  & \m2.83  & \m4.34  & \m6.14  & \m8.09  & \m9.90  & $-$      & \m5.76  & \\[2pt]
 & $\mu_d$                           & \m0.867 & \m0.864 & \m0.855 & \m0.845 & \m0.834 & \m0.823 & 0.8574   & \m0.847 & \\[5pt]
 & $\mathcal{M}_{\mathrm{M1}}$ (fm)             & \m3.995 & \m3.989 & \m3.973 & \m3.955 & \m3.936 & \m3.918 & $-$      & \m3.979 & \\[5pt]
 & $\mathcal{M}_{\mathrm{GT}}$ (fm)             & \m4.887 & \m4.881 & \m4.864 & \m4.846 & \m4.827 & \m4.810 & $-$      & \m4.859 & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{VP}}$ (\%)   & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.45$ & $-0.44$ & $-$      & $-0.45$ & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:C}}$ (\%) & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & \m0.03  & $-$      & \m0.03  & \\[2pt]
 & $\delta_{\mathrm{1B}}^{\mathrm{C2:N}}$ (\%) & $-0.19$ & $-0.19$ & $-0.18$ & $-0.15$ & $-0.12$ & $-0.10$ & $-$      & $-0.21$ & \\
\hline
\end{tabular*}\\[2pt]
The experimental values are given in ref. \cite{Eato75}.
\end{sidewaystable}

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\subsection{Useful table packages}

Modern \LaTeX{} comes with several packages for tables that
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\begin{description}
  
\item[\texttt{array}] Various extensions to \LaTeX's \texttt{array}
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\item[\texttt{longtable}] Automatically break tables over several
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\item [\texttt{dcolumn}] Define your own type of column. Among others,
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\item[\texttt{tabularx}] Smart column width calculation within a
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\end{description}


\subsection{PostScript figures}

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\begin{figure}[htb]
\vspace{9pt}
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Good sharp prints should be used and not (distorted) photocopies.}
\label{fig:largenenough}
\end{figure}
%
\begin{figure}[htb]
\framebox[55mm]{\rule[-21mm]{0mm}{43mm}}
\caption{Remember to keep details clear and large enough.}
\label{fig:toosmall}
\end{figure}


\section{EQUATIONS}

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\begin{thebibliography}{9}

\bibitem{mmt} "Can Centauros or Chirons be the first observations of 
evaporating mini black holes?", A.Mironov, A.Morozov and T.N.Tomaras;
hep-ph/0311318.
\bibitem{ewa} E.Gladysz-Dziadu\'s, hep-ph/0111163, and references therein.
\bibitem{OST} A.Ohsawa, Shibata and M.Tamada,............................. 
\bibitem{cct} A.Cafarella, C.Corian\`o and T.N.Tomaras, ``Cosmic Ray Signals
from Mini Black Holes in models with Extra Dimensions: An Analytical/Monte Carlo
study'', hep-ph/0410358.
\bibitem{cct2} A.Cafarella, C.Corian\`o and T.N.Tomaras, ``Searching for Extra
Dimensions in High Energy Cosmic Rays'', hep-ph/0410190. Talk presented in this
meeting by Claudio Corian\'o.
\bibitem{wb} E.Waxman and J.N.Bahcall, Phys. Rev. {\bf D59} (1999) 023002;
hep-ph/9902383.
\bibitem{w} E.Waxman, Nucl. Phys. Proc. Suppl. {\bf 118} (2003) 353.
\bibitem{kalashev} O.E.Kalashev, V.A.Kuzmin, D.V.Semikoz and G.Sigl,
Phys. Rev. {\bf D66} (2002) 063004.
\bibitem{ewa2} E.Gladysz-Dziadu\'s, hep-ph/0403.....................
\bibitem{cir} D.Chialva, R.Iengo and J.Russo, hep-th/0310283.

\end{thebibliography}

References should be collected at the end of your paper. Do not begin
them on a new page unless this is absolutely necessary. They should be
prepared according to the sequential numeric system making sure that
all material mentioned is generally available to the reader. Use
\verb+\cite+ to refer to the entries in the bibliography so that your
accumulated list corresponds to the citations made in the text body. 

Above we have listed some references according to the
sequential numeric system \cite{Scho70,Mazu84,Dimi75,Eato75}.
\end{document}

hep-ph0411081.extracted_bib
\begin{thebibliography}{9}
\bibitem{Scho70} S. Scholes, Discuss. Faraday Soc. No. 50 (1970) 222.
\bibitem{Mazu84} O.V. Mazurin and E.A. Porai-Koshits (eds.),
                 Phase Separation in Glass, North-Holland, Amsterdam, 1984.
\bibitem{Dimi75} Y. Dimitriev and E. Kashchieva, 
                 J. Mater. Sci. 10 (1975) 1419.
\bibitem{Eato75} D.L. Eaton, Porous Glass Support Material,
                 US Patent No. 3 904 422 (1975).
\end{thebibliography}