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\begin{titlepage}
\pubdate{\today}                    %fill in the date
\pubnumber{CERN-TH/2001-345 \\ FTUAM 01/22 
\\ IFT-UAM/CSIC-01-38 \\ IPPP/01/57\\ DCPT/01/112} %preprint number(s)
\vfill
\Title{Large dark matter cross sections from supergravity and superstrings}
\vfill
\Author{D. G. Cerde\~no}
%%
%%\address{Departamento de F\'{\i}sica
%%Te\'orica C-XI, Universidad Aut\'onoma de Madrid,
%%Cantoblanco, 28049 Madrid, Spain. }
%
%\footnote{And possible funding acknowledgements.
%                           DELETE THIS FOOTNOTE IF UNNECESSARY!!}
% }
\Address{Departamento de F\'{\i}sica
Te\'orica C-XI, Universidad Aut\'onoma de Madrid,\\
         Cantoblanco, 28049 Madrid, Spain.}
\vfill
%\andauth
\vfill
\Author{S. Khalil}
\Address{IPPP, Physics Department, Durham University, 
%\\
         DH1 3LE, Durham, U.K.}
\Address{Ain Shams University, Faculty of Science, Cairo, 11566, Egypt.}
\vfill
\andauth
\vfill
\Author{C. Mu\~noz}
\Address{Theory Division, CERN, CH-1211 GENEVA 23, Switzerland.}
\Address{
Departamento de F\'{\i}sica
Te\'orica C-XI and Instituto de F\'{\i}sica
Te\'orica C-XVI, Universidad Aut\'onoma de Madrid, 
Cantoblanco, 28049 Madrid, Spain.}
\vfill
\begin{Abstract}
We study the direct detection of supersymmetric dark
matter in the light of recent experimental results. In particular, 
we show that regions in the parameter space of
several scenarios with a 
neutralino-nucleon cross section of the order of $10^{-6}$ pb,
i.e., where current dark matter detectors are sensitive, can be
obtained. 
These are supergravity scenarios 
%with large 
%$\tan \beta$, with non-universal soft supersymmetry-breaking terms, 
%with multi-TeV masses for scalar superpartners known as 
%`focus point' supersymmetry, 
%and finally scenarios 
with intermediate unification 
scale, and superstring scenarios with D-branes.
\end{Abstract}
\vfill
\begin{Presented}
    COSMO-01 \\
    Rovaniemi, Finland, \\
    August 29 -- September 4, 2001
\end{Presented}
\vfill
\end{titlepage}
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%\begin{document}

%\title{Supersymmetric dark matter and neutralino-nucleon cross
%section
%%\footnote{Plenary review talk given
%%by C. Mu\~noz 
%%at the CICHEP
%%2001}
%}

%%\author{D. G. Cerde\~no }
%%
%%\address{Departamento de F\'{\i}sica
%%Te\'orica C-XI, Universidad Aut\'onoma de Madrid,
%%Cantoblanco, 28049 Madrid, Spain. }
%%
%%\author{S. Khalil}
%%
%%\address{Centre for Theoretical Physics, University of Sussex,
%%Brighton BN1 9QJ, U.K.\\
%%Ain Shams University, Faculty of Science, Cairo, 11566, Egypt.}
%%
%%\author{C. Mu\~noz}
%%
%%\address{Departamento de F\'{\i}sica
%%Te\'orica C-XI and Instituto de F\'{\i}sica
%%Te\'orica C-XVI, Universidad Aut\'onoma de Madrid,
%%Cantoblanco, 28049 Madrid, Spain. }


%\rightline{FTUAM 01/10}
%\rightline{IFT-UAM/CSIC-01-16}
%%\rightline{HIP-2000-69/TH}
%\rightline{SUSX-TH/01-021}
%\rightline
%\rightline{May 2001}   

%\renewcommand{\thefootnote}{\fnsymbol{footnote}}
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%\vspace{0.0cm}
%\begin{center}
%{\large{\bf Supersymmetric dark matter and neutralino-nucleon 
%\\ cross section \footnote{Extension of a talk given at Cairo International
%Conference on High Energy Physics (CICHEP 2001), January 9-14.}\\[5mm]}}


%\sc{D.G. Cerde\~no}\\
%{\small
%{\it Departamento de F\'{\i}sica
%Te\'orica C-XI, Universidad Aut\'onoma de Madrid,\\
%Cantoblanco, 28049 Madrid, Spain. \\[5mm]}}
%\sc{S. Khalil}\\
%{\small
%{\it Centre for Theoretical Physics, University of Sussex, 
%Brighton BN1 9QJ, U.K.\\
%\it  Ain Shams University, Faculty of Science, Cairo
%11566, Egypt.}}\\[5mm]
%\sc{C. Mu\~noz}\\
%{\small
%{\it  Departamento de F\'{\i}sica
%Te\'orica C-XI and Instituto de F\'{\i}sica Te\'orica C-XVI,\\ 
% Universidad Aut\'onoma de Madrid,
%Cantoblanco, 28049 Madrid, Spain. \\}}


%\end{center}

%%\begin{center}
%%{\small
%%{\it $^1$ Departamento de F\'{\i}sica
%%Te\'orica C-XI, Universidad Aut\'onoma de Madrid,\\[-0.1cm]
%%Cantoblanco, 28049 Madrid, Spain. \\
%%\vspace*{2mm}
%%\it $^2$ Instituto de F\'{\i}sica Te\'orica  C-XVI,
%%Universidad Aut\'onoma de Madrid,\\[-0.1cm]
%%Cantoblanco, 28049 Madrid, Spain.\\
%%\vspace*{2mm}
%%\it $^3$ Centre for Theoretical Physics, University of Sussex, 
%%Brighton BN1 9QJ, U.K.\\
%%\vspace*{2mm}
%%\it $^4$ Ain Shams University, Faculty of Science, Cairo
%%11566, Egypt.} 
%%}
%%\end{center}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
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%\renewcommand{\thefootnote}{\alph{footnote}}
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%%\abstract
%{\small We review the direct detection of supersymmetric dark
%matter in the light of recent experimental results. In particular, 
%we show that regions in the parameter space of
%several supergravity scenarios with a 
%neutralino-nucleon cross section of the order of $10^{-6}$ pb,
%i.e., where current dark matter detectors are sensitive, can be
%obtained. 
%These are scenarios with large 
%$\tan \beta$, with non-universal soft supersymmetry-breaking terms, 
%with multi-TeV masses for scalar superpartners known as 
%`focus point' supersymmetry, 
%and finally scenarios with intermediate unification 
%scale which appear naturally in some superstring constructions.}



\section{\large Introduction}
%One of the strongest motivations for physics beyond the standard model is the
%existence of dark matter. Substantial evidences suggest that most
%of the mass in the Universe is some non-luminous matter, the so called
%`dark matter' \cite{contemporary}.
%A key question is then, what 
%could this dark matter be? We don't know the answer
%yet, but we do know that not all of it can be ordinary (baryonic) matter,
%% (not formed from neutrons and protons), 
%since measured abundances of helium, deuterium and lithium in the 
%scenario of big-bang nucleosynthesis 
%impose a strong upper bound on the baryon density in the Universe. This 
%density
%%$\Omega_b =\rho_b/\rho_c < 0.1$, where $\rho_c \simeq 10^{-29}
% %g/cm^3$, 
%is too small to account for the whole dark matter in the Universe. 
%The conclusion is that baryonic objects, such as e.g. MACHOs, 
%can be components of the dark matter, but more candidates are 
%needed.

%Fortunately, 
%particle physics offers various candidates for (non-baryonic) dark matter,
%all of which would indicate new physics beyond the well tested standard model
%of particle physics \cite{contemporary}. 
One of the most interesting
candidates for dark matter is a  
long-lived or stable weakly-interacting massive 
particle (WIMP). WIMPs can remain from the earliest moments of the Universe in 
sufficient number to account for a significant fraction of relic density. 
These particles would form not only a background density in the Universe, but
also would cluster gravitationally with ordinary stars in the galactic halos.

This raises the hope of detecting relic 
WIMPs directly, by observing their elastic scattering on  
target nuclei through nuclear recoils.
Since WIMPs interact with ordinary matter with very roughly weak
strength, and assuming that their masses are of the order of  
weak scale (i.e., between 10 GeV and a few TeV),
it is natural to expect a WIMP-nucleus cross section of the same order
as that of a weak process, which is around 1 pb.
This would imply a WIMP-nucleon cross section around   
$10^{-8}$ pb, too low to be detected by current dark matter
experiments,
which are sensitive to a cross section around $10^{-6}$ pb.
Surprisingly, 
the DAMA collaboration reported recently \cite{experimento1}
data favouring the existence of a 
WIMP signal in their search for annual modulation.
When 
uncertainties as e.g. the WIMP velocity or possible bulk halo rotation,
are included, it was claimed that the preferred range of parameters
is  (at 4$\sigma$ C.L.) $10^{-6}$ pb $\lsim \sigma\lsim 10^{-5}$ pb 
for a WIMP mass 30 GeV $\lsim m \lsim 200$ GeV.
However,
unlike this spectacular result, the CDMS collaboration 
claims to have excluded \cite{experimento2} regions of the DAMA 
parameter space.

Given these intriguing experimental results, it is then
crucial to re-analyze the compatibility of WIMPs as dark matter
candidates, with the sensitivity of current dark matter detectors.
To carry this analysis out we have to assume a particular candidate
for WIMP.
The leading candidate in this class is the lightest 
neutralino \cite{contemporary}, a particle 
predicted by the supersymmetric (SUSY) extension of the standard model.

In particular, in 
the 
minimal supersymmetric standard model (MSSM)
there are four neutralinos, $\tilde{\chi}^0_i~(i=1,2,3,4)$, since they
are the physical 
superpositions of the fermionic partners of the neutral electroweak 
gauge bosons, 
called bino ($\tilde{B}^0$) and wino ($\tilde{W}_3^0$), and of the
fermionic partners of the  
neutral Higgs bosons, called Higgsinos ($\tilde{H}^0_u$, 
$\tilde{H}_d^0$). 
Therefore the lightest neutralino, $\tilde{\chi}^0_1$, will be the 
dark matter candidate.
We parameterize the gaugino and Higgsino content
of the lightest neutralino according to 
%
\begin{equation}
\tilde{\chi}^0_1 = N_{11} \tilde{B}^0 +N_{12} \tilde{W}_3^0 +
N_{13} \tilde{H}^0_d + N_{14} \tilde{H}^0_u\ .
\label{lneu}
\end{equation}
%
It is commonly defined that $\tilde{\chi}^0_1$ is mostly gaugino-like 
if $P\equiv \vert N_{11}\vert^2 + \vert N_{12} \vert^2 > 0.9$, Higgsino-like
if $P<0.1$, and mixed otherwise.











%Recently, the DAMA collaboration reported data favouring the existence of a 
%WIMP signal in their search for annual modulation. When WIMP velocity
%uncertainties are included, it was claimed that the preferred range of
%parameters is  $10^{-6} \lsim \sigma_{\tilde{\chi}^0_1 -p} \lsim 10^{-5}$ 
%for $30 \lsim m_{\tilde{\chi}^0_1} \lsim 200$ (3$\sigma$ CL). However, 
%the new 90\% CL CDMS experiment limit excludes the 3$\sigma$ DAMA region at 
%more than 84\% CL. 


%\section{\large Supersymmetric predictions for the neutralino-nucleon cross section}

%In SUSY models, $R$-parity is often imposed to avoid weak scale 
%proton decay or lepton number violation. Imposing this symmetry yields 
%remarkable phenomenological implications. SUSY particles are produced 
%or destroyed only in pairs and, as a consequence, the lightest 
%supersymmetric particle (LSP) 
%is absolutely stable.
%The former implies that
%a major signature 
%for $R$-parity conserving models is represented by events with missing 
%energy (for instance, $e^+ e^- \rightarrow \mathrm{jet}+ \mathrm{ missing\ 
%energy}$). The latter implies that the LSP 
%might constitute a possible candidate for dark matter. 
%Concerning this point, it is remarkable that in most of the parameter
%space of SUSY models the LSP is an electrically neutral 
%(also with no strong interactions) particle, called neutralino.
%This is welcome since otherwise the LSP 
%would bind to nuclei and would be excluded as a candidate
%for dark matter from unsuccessful searches for exotic heavy 
%isotopes \cite{isotopes}.


%In the simplest SUSY extension of the standard model, the so-called
%minimal supersymmetric standard model (MSSM)
%there are four neutralinos, $\tilde{\chi}^0_i~(i=1,2,3,4)$, since they
%are the physical 
%superpositions of the fermionic partners of the neutral electroweak 
%gauge bosons, 
%called bino ($\tilde{B}^0$) and wino ($\tilde{W}_3^0$), and of the
%fermionic partners of the  
%neutral Higgs bosons, called Higgsinos ($\tilde{H}^0_u$, 
%$\tilde{H}_d^0$). 
%Therefore the lightest neutralino, $\tilde{\chi}^0_1$, will be the 
%dark matter candidate.
%The neutralino mass matrix 
%with the conventions for gaugino and Higgsino masses in the Lagrangian,
%${\cal L} =\frac{1}{2}\sum_{a} M_a {\lambda}_a \lambda_a + 
%\mu \tilde{H}^0_u \tilde{H}^0_d$ + h.c.,
%is given by
%%
%\begin{equation}
%{\small \bmat{cccc}M_1 & 0 &-M_Z\cos\beta \sin\theta_W &M_Z\sin\beta 
%\sin\theta_W \\ 0 & M_2 & M_Z \cos \beta \cos\theta_W & -M_Z \sin \beta 
%\cos\theta_W \\ -M_Z \cos \beta \sin\theta_W & M_Z \cos \beta\cos\theta_W&
%0& -\mu \\ M_Z \sin \beta \sin\theta_W & -M_Z \sin \beta\cos\theta_W&-\mu 
%& 0 \emat,}
%\label{mass}
%\end{equation}
%%
%in the above basis 
%($\tilde B^0=-i{\lambda}'$, $\tilde W_3^0=-i{\lambda}^3$, $\tilde H_u^0$, 
%$\tilde H_d^0$). 
%%and with the convention in the superpotential
%%$W=-\mu \epsilon_{ij} H_d^i H_u^j = -\mu (H_d^0 H_u^0-H_d^- H_u^+)$.
%Here $M_1$ and $M_2$ are the soft bino and wino masses respectively, 
%$\mu$ is the Higgsino mass parameter 
%and 
%$ \tan\beta= \langle H_u^0\rangle/\langle H_d^0\rangle$ 
%is the ratio of Higgs vacuum expectation values. 
%We parameterize the gaugino and Higgsino content
%of the lightest neutralino according to 
%%
%\begin{equation}
%\tilde{\chi}^0_1 = N_{11} \tilde{B}^0 +N_{12} \tilde{W}_3^0 +
%N_{13} \tilde{H}^0_d + N_{14} \tilde{H}^0_u\ .
%\label{lneu}
%\end{equation}
%%
%It is commonly defined that $\tilde{\chi}^0_1$ is mostly gaugino-like 
%if $P\equiv \vert N_{11}\vert^2 + \vert N_{12} \vert^2 > 0.9$, Higgsino-like
%if $P<0.1$, and mixed otherwise.

%The relevant effective Lagrangian describing
%the elastic $\tilde{\chi}^0_1$-nucleon scattering in the MSSM is given by
%%
%\begin{equation}
%\mathcal{L}_{eff} = \sum_{q} \left(\alpha_{q} \bar{\chi}\chi \bar{q} q
%+
%\beta_q \bar{\chi} \gamma^{\mu}  \gamma^{5} 
%\chi \bar{q} \gamma_{\mu}  \gamma^{5} q\right)\ ,
%\end{equation}
%%
%where  $\alpha_q$, $\beta_q$ are given e.g. in ref.\cite{Ellis} 
%with the sign conventions for Yukawa couplings in the Lagrangian,
%${\cal L}=-h_u H_u^0 \bar u_L u_R -h_d H_d^0 \bar d_L d_R 
%- h_e H_d^0 \bar e_L e_R $ + h.c.,
%and the sum 
%runs over the six quarks. 
%The contribution of the scalar (spin-independent) interaction,
%the one proportional to $\alpha_q$, to the $\tilde{\chi}^0_1$-nucleon 
%cross section is generically larger than the spin-dependent
%interaction,
%the one proportional to $\beta_q$.
%One can concentrate then on the scalar 
%%In particular, in the context of DAMA and CDMS experiments,
%% $\sigma_{spin}/\sigma_{scalar} \sim 1-5 \%$. 
%$\tilde{\chi}^0_1$-nucleon
%cross section. This is given by
%%
%\begin{equation}
%\sigma
%%_{\tilde{\chi}_1^0-p} 
%= \frac{4 m_{r}^2}{\pi} f^2\ ,
%\label{crosssection}
%\end{equation}
%%
%where $m_{r}$ is the reduced $\tilde{\chi}^0_1$ mass and
%%
%\begin{equation}
%\frac{f}{m} = \sum_{q} f_q \frac{\alpha_q}{m_q}
%\end{equation}
%%
%with $m$ the mass of the nucleon and $m_q$ the mass of the quarks. 
%The scalar 
%coefficients $\alpha_{q}$ include contributions from 
%squark ($\tilde q$) exchange and neutral Higgs 
%$(h, H)$ exchange, as illustrated in Fig.~\ref{Feynman}.  
%The numerical values of the hadronic matrix elements $f_q$ 
%for the proton are as follows \cite{Ellis}:
%%
%\begin{equation}
%f_u= 0.020 \pm 0.004\ , \hspace{0.5cm} f_d= 0.026 \pm
%0.005\ ,
%\hspace{0.5cm} f_s= 0.118 \pm 0.062\ ,
%\label{central}
%\end{equation}
%%
%and \footnote{Larger values,
%as for example $f_s=0.455$, have also been used in the 
%literature, see e.g. ref.~\cite{Arnowitt}.} 
%$f_{c,b,t}= \frac{2}{27} (1-\sum_{q=u,d,s} f_q)$.
%For the neutron the value of $f_s$ is the same and therefore
%the scalar cross sections for both, protons and neutrons, are
%basically equal. 

%\begin{figure}[t]
%\begin{center}
%%\includegraphics[height=1.5in]{feynman.eps}
%\epsfig{file= feynman.eps,height=3.5cm,angle=0}
%\end{center}
%\caption{Feynman diagrams contributing to neutralino-nucleon cross section.}
%\label{Feynman}
%\end{figure}




The cross section for the elastic scattering of relic neutralinos on 
protons and neutrons has been examined exhaustively in the 
literature \cite{kami}.   
This is for example the case in
the framework of minimal supergravity (mSUGRA).
Let us recall that in this framework one makes several 
assumptions. In particular, 
the scalar mass parameters, the gaugino mass parameters, and the 
trilinear couplings, which are generated once SUSY is broken through
gravitational interactions, are universal at the 
grand unification 
scale, $M_{GUT} \approx 2\times 10^{16}$ GeV.
They are denoted by $m_0$, $M_{1/2}$, and $A_0$ respectively. 
Likewise, 
radiative electroweak symmetry breaking is imposed, i.e., 
the Higgsino mass parameter $\mu$ is 
determined by the minimization of the Higgs effective 
potential. This implies 
% 
\begin{equation}
\mu^2 = \frac{m_{H_d}^2 - m_{H_u}^2 \tan^2 \beta}{\tan^2 \beta -1 } - 
\frac{1}{2} M_Z^2\ ,
\label{electroweak}
\end{equation} 
%
where 
$\tan\beta= \langle H_u^0\rangle/\langle H_d^0\rangle$ 
is the ratio of Higgs vacuum expectation values. 
With these assumptions, the mSUGRA framework  allows four free 
parameters: $m_0$, $M_{1/2}$, $A_0$, and $\tan \beta$. In addition, the
sign of $\mu$ 
remains also undetermined.  

%\begin{figure}[t]
%\begin{center}
%%\includegraphics[height=1.5in]{running2.eps}
%\epsfig{file= running2.eps,width=7cm,height=3.5cm,angle=0}
%\end{center}
%\caption{
%Running of the soft Higgs masses-squared with energy.}
%\label{run}
%\end{figure}





It was observed (for a recent re-evaluation see ref.\cite{Ellis})
that for low and moderate values of
$\tan \beta$ the lightest neutralino is 
mainly bino, and therefore the 
predicted scalar neutralino-proton cross sections
are well below the accessible experimental regions.
%To understand this result qualitatively, we show schematically in
%Fig.~\ref{run} 
%the well known evolution of $m_{H_d}^2$ and $m_{H_u}^2$ with the
%scale
%%\footnote{Let us remark that, given the convention used throughout
%%this review for gaugino masses in the Lagrangian, 
%%${\cal L} =\frac{1}{2}\sum_{a} M_a {\lambda}_a \lambda_a$ + h.c., we
%%are using the renormalization group equations (RGEs) obtained e.g.
%%in ref.\cite{rges}, but with an opposite sign in the
%%gaugino contributions to the RGE's of the $A_0$ parameters.}. 
%Since $m_{H_u}^2$ becomes large and negative (notice also
%that $m_{H_d}^2$, neglecting
%bottom and tau Yukawa couplings, becomes positive), $|\mu|$ due
%to relation (\ref{electroweak}) 
%becomes also large, in particular much larger than
%$M_1$ and $M_2$. Thus, as can be easily understood,
%%from 
%%eqs.(\ref{mass}) and (\ref{lneu}), 
%the lightest neutralino will be mainly gaugino, and in particular
%bino since at low energy $M_1\approx \frac{1}{2}M_2$.
In particular,
%As we can see in the figure
%although the cross section increases when 
%the value of $\tan \beta$ increases, still for $\tan \beta=20$  
$\sigma_{\tilde{\chi}_1^0-p} \lsim 10^{-7}$ pb, and
therefore
%for these values of the parameters
%Given this situation, 
we would have to wait in principle for projected detectors,
as e.g. GENIUS \cite{GENIUS}, 
to be able to
test the neutralino as a dark-matter candidate.




%We show this fact in Fig.~\ref{ellisfig}a, 
%where for $\tan\beta=3$ the gaugino-Higgsino 
%components-squared $N_{1i}^2$ of the lightest neutralino as a function
%of its mass $m_{\tilde{\chi}_1^0}$ 
%are exhibited. Here we are using as an example $m_0=150$ GeV, and
%$M_{1/2}$ is essentially fixed for a given
%$m_{\tilde{\chi}_1^0}$.
%Note that 
%%$m_{\tilde{\chi}_1^0}>70$, 
%$N_{11}$ is 
%extremely large and therefore $P\gsim 0.9$.
%Then, the scattering channels through Higgs exchange shown in 
%Fig.~\ref{Feynman} are suppressed (recall that the Higgs-neutralino-neutralino
%couplings are proportional to $N_{13}$ and $N_{14}$) and therefore
%the cross section is small.
%As a matter of fact, the scattering channels through squark 
%exchange, shown also in Fig.~\ref{Feynman}, 
%are also suppressed by the mass of the squarks. Indeed
%in this limit the cross section (\ref{crosssection}) can be approximated as
%%
%\bea
%\sigma_{\tilde\chi_1^0-p}
%\approx {m_r^2}\ \frac{\alpha^2}{\left(m_{\tilde s}^2-
%m_{\tilde{\chi}_1^0}^2\right)^2}\  f_s^2\   |N_{11}|^4
%\ .
%\label{cross}
%\eea
%%
%Thus it can be roughly estimated to be 
%$\sigma_{\tilde{\chi}_1^0-p}\approx 10^{-8}$ pb,
%for $\alpha\approx 10^{-2}$, 
%$f_s\approx 10^{-1}$,
%$m_r\approx 1$ GeV and 
%$m_{\tilde s}\approx 300$ GeV. This is precisely the value of
%the cross section 
%expected for a weak process as discussed in the Introduction.


%%
%\begin{figure}[t]
%\begin{center}
%\epsfig{file= elliscomponents.eps,
%%width=11cm,
%height=7cm
%}
%%\hspace{0.5cm}\epsfig{file=ellis_m30-550.eps, width=5.75cm, height=4.5cm
%%,angle=0
%% }
%\end{center}

%\vspace{-0.5cm}

%\caption{(a) Gaugino-Higgsino components-squared
%%$N_{1i}^2$ 
%of the lightest neutralino as a function of its mass.
%%for the case
%%$\tan\beta=10$, $M_I=10^{16}$ GeV and
%%$M_I=10^{11}$ GeV
%(b) 
%Scatter plot of the neutralino-proton cross section
%%$\sigma_{\tilde{\chi}_1^0 P}$ 
%as a function of 
%the neutralino mass for the scenario discussed in the text.
%%$m_{\tilde{\chi}_1^0}$
%DAMA and CDMS current 
%experimental limits and projected GENIUS limits are shown.
%}
%\label{ellisfig}
%\end{figure}
%%




%In Fig.~\ref{ellisfig}b we show the cross section
%$\sigma_{\tilde{\chi}_1^0-p}$ as a function of the neutralino mass
%$m_{\tilde{\chi}_1^0}$ for
%$\tan \beta=3$.
%We also choose to plot only the case $\mu > 0$ since for negative values of
%$\mu$ the cross sections are much
%smaller\footnote{It is also worth
%noticing that constraints
%coming from
%the $b\rightarrow s\gamma$ process highly reduce
%the $\mu<0$ parameter space. In addition,
%recent measurements of the anomalous magnetic moment of the
%muon \cite{marci} seems to exclude all cases with $\mu<0$.}.
%%In what follows we will always use
%%$\mu > 0$.
%Fig.~\ref{ellisfig}b has been obtained
%using formula (\ref{crosssection}) with the central
%values for the hadronic matrix elements given by
%eq.(\ref{central}). We will use these values throughout this
%review\footnote{It is worth mentioning here that values for the hadronic matrix
%elements as those discussed in footnote {\it a}
%will increase in one order of magnitude the results of this and
%the other figures in this review,
%%Fig.~\ref{arnowit},
%since their contribution appears raised to the square
%in eq.(\ref{crosssection}).}.
%Likewise we impose
%the present
%bounds coming from accelerators.
%These are
%LEP and Tevatron bounds on SUSY masses and
%CLEO $b\to s\gamma$ branching ratio measurements.
%For the Higgs mass we use the present experimental
%lower limit for $\tan\beta=3$ \cite{lep}, i.e. $m_h>95$ GeV.
%Although, for the values of $\tan\beta$ that we will
%consider in the next section, $\tan\beta=10$,
%this limit is considerably weaker \cite{lep},
%$m_h>80$ GeV, we will still use $m_h>95$ GeV.
%%and there will be no constraint on $m_{\tilde{\chi}_1^0}$.
%Concerning the parameter space of the figure, we have used
%30 GeV $\leq m_0 \leq 550$ GeV, where the lower bound 
%is in order to avoid the stau being the LSP for all values of 
%$m_{\tilde{\chi}_1^0}$.
%Note that the curve associated to $m_0=550$ GeV 
%corresponds to the minimum values of 
%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ in the figure.
%On the other hand, since the cross sections are not very sensitive to 
%the specific values of $A_0$ in a wide 
%range (we have checked that 
%this is so for $\mid A_0/M_{1/2}\mid \lsim 1$), we fix
%$A_0 = M_{1/2}$ in the figure.
%%and $m_0$ 
%As mentioned above 
%the gaugino mass
%$M_{1/2}$ is essentially fixed for a given $\tan\beta$ and 
%$m_{\tilde{\chi}_1^0}$. 
%For this figure we have to take
%140 GeV $\lsim M_{1/2} \lsim 350$ GeV,
%where the lower bound, corresponding to $m_{\tilde{\chi}_1^0}\geq 55$ GeV,
%is due to the experimental bound
%on the lightest chargino mass
%$m_{\tilde\chi_1^{\pm}}>90$ GeV. 
%%corresponding
%%to $m_{\tilde{\chi}_1^0}\geq 55$ GeV,
%%and the upper bound is because we choose to draw only  
%%$m_{\tilde{\chi}_1^0}\leq 200$ GeV.
%Negative values of $M_{1/2}$, not shown in the
%figure,
%correspond to smaller cross sections.


%%Let us finally remark that the cross sections are 
%%%and in order to 
%%%have it of order $10^{-6}$ one needs to used larger values for 
%%%$\tan \beta$ which we will consider in more details in the next section. 
%%sensitive 
%%to the sign of $\mu$ and, in particular, 
%%for $\mu < 0$ the cross sections are much 
%%smaller\footnote{It is also worth 
%%noticing that constraints 
%%coming from  
%%the $b\rightarrow s\gamma$ process highly reduce 
%%the $\mu<0$ parameter space. In addition, 
%%recent measurements of the anomalous magnetic moment of the
%%muon \cite{marci} seems to exclude all cases with $\mu<0$.}. 
%%In what follows we will always use
%%$\mu > 0$.




%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%\begin{figure}[t]
%%\begin{center}
%%\epsfig{figure=ellis2_m=30-550.eps, width=9cm, height=6.5cm}
%%\end{center}
%%\caption{
%%Neutralino-proton cross section
%%%$\sigma_{\tilde{\chi}_1^0 P}$ 
%%as a function of 
%%the neutralino mass
%%%$m_{\tilde{\chi}_1^0}$
%%for different values of $\tan\beta$. DAMA and CDMS current 
%%experimental limits and projected GENIUS limits are shown.}
%%\label{ellisfig}
%%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%





%As we can see in the figure
%%although the cross section increases when 
%%the value of $\tan \beta$ increases, still for $\tan \beta=20$  
%$\sigma_{\tilde{\chi}_1^0-p} \lsim 10^{-7}$ pb, and
%therefore
%for these values of the parameters
%%Given this situation, 
%we would have to wait in principle for the 
%projected GENIUS detector \cite{GENIUS} to be able to
%test the neutralino as a dark-matter candidate.

Recently, several proposals have been made in order to modify this
result, enhancing the neutralino-nucleon cross section.
This is the case of scenarios with large 
$\tan \beta$ \cite{Bottino}-\cite{Mario}, with
non-universal soft SUSY-breaking terms \cite{Bottino,Arnowitt,Nath2}, 
with multi-TeV masses
for scalar superpartners known as `focus point' 
supersymmetry \cite{focus}, 
with intermediate unification scale \cite{muas},
and
finally superstring scenarios with D-branes 
\cite{khalil,Nath2,Arnowitt2,bailin,nosotros}. 
In these proceedings we will concentrate only
on the last two.
A recent review where all the above mentioned scenarios are critically
reappraised can be found in ref.\cite{darkcairo}.



\section{\large Scenarios with intermediate unification scale}
 
%Recently there has been some theoretical 
%activity \cite{Bottino}-\cite{nosotros} trying to obtain regions
%in the parameter space of supergravity (SUGRA) scenarios 
%compatible with the sensitivity of
%current dark matter detectors, DAMA and CDMS. 
%The key point in most of these scenarios 
%to carry it out consists of reducing the value of $|\mu|$.
%Following the discussion below eq.(\ref{electroweak}) in the previous section, 
%the smaller $|\mu|$ is,
%the larger the Higgsino components of the lightest neutralino become.
%Eventually, $|\mu|$ will be of the order of $M_1$, $M_2$
%and $\tilde{\chi}_1^0$ will be a mixed Higgsino-gaugino state.
%Indeed scattering channels through Higgs exchange in 
%Fig.~\ref{Feynman}
%are now important and their contributions to the cross section
%(\ref{crosssection}) can
%be schematically approximated as 
%%
%\bea
%\sigma_{\tilde\chi_1^0-p}
%\approx {m_r^2}\
%\frac{\lambda_s^2 \alpha}{m_h^4}\
%f_s^2\   |N_{13} N_{11}|^2 
%\ ,
%\label{cross2}
%\eea
%%
%where $\lambda_s$ is the strange quark Yukawa coupling and
%$m_h$ represent the Higgs masses.
%With the same rough estimate as in eq.(\ref{cross}),
%one obtains $\sigma_{\tilde{\chi}_1^0-p}\approx 10^{-6}$ pb for 
%$m_h\approx 100$ GeV.






%In this section we review the different SUGRA scenarios 
%that can be found in the
%literature in order to enhance the neutralino-proton cross section
%$\sigma_{\tilde\chi_1^0-p}$ to be of the order of $10^{-6}$ pb.




%\subsection{\normalsize Scenario with large $\tan \beta$}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%\begin{figure}[t]
%\begin{center}
%\epsfig{figure=ellis2_m30-550.eps, 
%%width=9cm, 
%height=7cm}
%\end{center}

%\vspace{-0.5cm}

%\caption{The same as in Fig.~\ref{ellisfig}b but for 
%$\tan\beta=10$ and 20.
%%Neutralino-proton cross section
%%as a function of 
%%the neutralino mass
%%for different values of $\tan\beta$. DAMA and CDMS current 
%%experimental limits and projected GENIUS limits are shown.
%}
%\label{ellisfig2}
%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%





%In the previous section we showed in Fig.~\ref{ellisfig}b
%the neutralino-proton cross section for $\tan\beta=3$, in the framework 
%of mSUGRA.
%Here we show the same in Fig.~\ref{ellisfig2} but for larger values of
%$\tan\beta$,
%in particular for  $\tan\beta=10$ (green points) and 20 (red points).
%We see 
%that the cross section increases when the value
%of $\tan\beta$ increases.
%For moderate values of $\tan\beta$, 
%%$\tan\beta\lsim 10$,
%the reason being that the top(bottom) Yukawa coupling
%which appears in the RGE
%for $m_{H_u}^2$($m_{H_d}^2$)
%decreases(increases) since it is proportional
%to $\frac{1}{\sin\beta}$($\frac{1}{\cos\beta}$).
%This implies that the negative(positive) contribution 
%$m_{H_u}^2$($m_{H_d}^2$) to $\mu^2$ in eq.(\ref{electroweak}) 
%is less important, and 
%therefore $|\mu|$ decreases. 
%%Notice e.g. that in 
%%Fig.~\ref{ellisfig}a, $P<0.9$ for 
%%$m_{\tilde{\chi}_1^0}< 70$ GeV.

%However, for $\tan\beta \gsim 10$, the value of $\mu^2$ is very
%stable with respect to variations of $\tan\beta$.
%This is due to the fact 
%that $\mu^2\approx -m_{H_2}^2 - \frac{1}{2}M_Z^2$ (see
%eq.(\ref{electroweak})). Since $\sin\beta\approx 1$, the top Yukawa
%coupling is stable and therefore the same conclusion is obtained for
%$m_{H_2}^2$ and $\mu^2$. Thus, 
%the reason for the cross section to increase
%when $\tan\beta$ increases
%cannot be now the increment of the Higgsino components of the LSP.
%Nevertheless there is a second effect in the cross section 
%which is now the dominant one: the contribution of the down-type
%quark Yukawa couplings (see eq.(\ref{cross2})) 
%which are proportional to $\frac{1}{\cos\beta}$.





%It was in fact
%pointed out in refs.\cite{Bottino,Arnowitt} that the large
%$\tan\beta$ regime allows regions where 
%$\sigma_{\tilde{\chi}_1^0-p}\approx 10^{-6}$ pb is reached. 
%We can see in Fig.~\ref{ellisfig2} that this is so for 
%$\tan\beta \gsim 20$.


%%As we have emphasized above, the current experiments sensitive to 
%%$\sigma_{\tilde\chi_1^0-p}\gsim 10^{-6}$ Pb are probing only large 
%%$\tan \beta$ regime for mSUGRA model, \ie~ $\tan \beta \gsim 25$.
%%However, at large $\tan \beta$, it is known that the stau mass--squared
%%matrix has a large off--diagonal mixing which makes the physical mass of the 
%%lightest stau signficantly lower than the mass of the other squarks and 
%%sleptons. Furthermore, the lightest stau mass eigenstate $\tilde{\tau}$
%%becomes the next lightest supersymmetric particle (NLSP) with mass 
%%splitting from the LSP could be of order one GeV, \ie~ 
%%$\Delta_{\tilde{\tau}_2} =(m_{\tilde{\tau}_2}-
%%m_{\tilde{\chi}_1^0})/m_{\tilde{\chi}_1^0} \sim 1$ GeV . Therefore, 
%%including the co-annihilation between the LSP and NLSP in computing
%%the LSP relic abundance is essential. Also it is known that the SUSY
%%correction to the bottom quark mass increase with $\tan\beta$. 
%%This correction originates mainly from squark/gluino and squark/chargino
%%loops and has a sign opposite to the one of $\mu$ .
%%Thus, for $\mu>0$, the corrected $m_b(m_Z)$ will be at the upper
%%limit experimentally allowed range. For $\mu<0$, however,  
%%there appears a large negative correction, which pushes the prediction for
%%$m_b(m_Z)$ towards the lower limit of the experimental data.
%%The choice  $\mu>0$ leads to a very mild constrain on $m_A$ coming from
%%$b\rightarrow s \gamma$. As a result the LSP can be relatively light and
%%the obtained detection rates are not suppressed. On the other hand for the
%%choice $\mu<0$ the experimental bounds on $b\rightarrow s \gamma$ can be
%%satisfied only for large values of $m_{\tilde{\chi}}$ \cite{cdm2} resulting
%%in very low detection rates. In this respect, the analysis of the 
%%LSP--neuclon cross section within a large $\tan\beta$ regime requires a 
%%carefull study which has performed in ref.\cite{Bottino,Arnowit,Mario}.

%%In this analysis it turns out that the LSP is mostly bino--like
%%with $P > 0.9$ (in the region of the parameter space where 
%%$\tilde{\chi}_1^0 -\tilde{\tau}$ co-annhilations effects are sizeable) and
%%even $p>0.95$ for $m_{\tilde{\chi}_1^0}>100$. 
%Very large values of 
%$\tan\beta$, 
%like $\tan \beta \simeq 50$ which 
%correspond approximately to the unification of the tau and top Yukawa 
%couplings at $M_{GUT}$,
%have also been considered \cite{Mario}.
%Although it was found, as expected, that the 
%cross section is enhanced,
%the 
%well known
%experimental limits coming from 
%$b \to s \gamma$ for large $\tan\beta$, 
%lead to severe constraints on the parameter space. In particular,
%these constraints imply $\sigma_{\tilde{\chi}_1^0-p} \lsim 
%10^{-6}$ pb. 
%%Furthermore it turns out that the LSP--relic density in 
%%this scenario is small (arround the lower bound in the region where 
%%the coannihilation is not valied and even much less than the lower bound in 
%%the coannihilation region). Furthermore, the LSP relic density in this 
%%scenario is very small. This suppression of $\Omega_{\tilde{\chi}_1^0} h^2$ 
%%is not due to any enhancement of the LSP's Higgsino component from large 
%%$\tan \beta$.  Rather it results from two enhancements to the
%%process $\tilde{\chi}_1^0 \tilde{\chi}_1^0 \to A \to f \bar{f}$.  
%%First, the $Af\bar{f}$ coupling is proportional to $\tan\beta$ for 
%%isospin $-\frac{1}{2}$ fermions.
%%Second, for large $\tan \beta$, the bottom Yukawa coupling $h_b$ becomes
%%significant and lowers $m_A$.

%%Therefore, and as pointed out in ref.\cite{arnowit} combining these 
%%constraints imples that the values of $\sigma_{\tilde{\chi}_1^0-p}$ at 
%%large $\tan \beta$ can be smaller than $\sigma_{\tilde{\chi}_1^0-p}$ at 
%%$\tan \beta \simeq3$.

%\subsection{\normalsize Focus point supersymmetry scenario}

%Another possibility 
%to obtain a large 
%neutralino-nucleon cross section 
%%and higher 
%%expected rates of detection appears 
%arises in the so-called focus point 
%supersymmetry scenario.
%This has been proposed \cite{Feng} 
%in order to avoid dangerous SUSY contributions to 
%flavour and CP violating effects.
%The idea is to assume the existence of squark and sleptons with
%masses which can be taken well 
%above\footnote{Of course this scenario rules out SUSY
%as an explanation of the
%possible deviation in the muon anomalous magnetic moment
%from the standard model prediction \cite{marci}.} 1 TeV.
%It has also been argued that this situation produces no loss of naturalness.

%The implications of focus point supersymmetry for neutralino dark matter
%have been considered in ref.\cite{focus}.
%%where one can avoids naturalness constraints with 
%%multi--TeV scalar masses~\cite{feng}. 
%%Although this scenario rules out 
%%supersymmetry as a possible explanation of the recently observed 
%%2.6 $\sigma$ deviation in the muon $g-2$ from the SM prediction, it is still
%%a possible way to enhance the neutralino--nucleon cross sections, as well show
%%below. In ref.\cite{feng} 
%In particular, it was pointed out that for 
%$m_0 > 1$ TeV, unlike the usual cases with $m_0 < 1$ TeV,  
%the lightest neutralino is a gaugino-Higgsino 
%mixture over much of parameter space.
%%and its relic abundances do not overclose the  Universe but
%%lie in the cosmologically interesting range.  
%%Also the detection rates may
%%be large with $\sigma_{\tilde{\chi}_1^0 -P} \approx 10^{-6}$. 
%Let us recall from the previous subsection 
%that for moderate and large values of $\tan\beta$,
%$\mu^2$ in eq.(\ref{electroweak}) can be approximated as 
%%In the focus point, the weak scale value of $m_{H_u}^2$ is insensitive to 
%%variations in SUSY parameters, even for multi--TeV $m_0$. For 
%%$\tan \beta \gsim 5$ the $\mu$ in eq.(\ref{electroweak}) is 
%%approximated as 
%%
%\begin{equation}
%\mu^2 \approx - m_{H_u}^2 - \frac{1}{2} M_Z^2. 
%\label{approxmu}
%\end{equation}
%%
%Thus 
%%for $m_0 < 1$ TeV, the RG evolution drives $m_{H_u}^2$ larger and
%%negative which by eq.(\ref{approxmu}) implies $\vert \mu \vert$ much larger
%%that $M_1$ and $M_2$, hence the LSP becomes nearly pure bino, with $P > 0.9$.
%%However, 
%for $m_0 > 1$ TeV, 
%%and for large or moderate values of $\tan \beta$ 
%%postitve corrections to 
%$m_{H_u}^2$ becomes less negative, and therefore $|\mu|$ decreases.
%%rendering it less negative. Thus  
%%if all other parameters are fixed, one finds that as $m_0$ increases, $|\mu|$
%%decreases, and eventually $|\mu| \sim M_1, M_2$, which leads to
%%significant mixing between Higgsino and gaugino states.  As $m_0$  
%%increases further, the Higgsino content of $\chi$ increases until
%%ultimately one enters the domain $|\mu| < 95$ GeV, which is excluded
%%by limits from chargino searches at LEP II.
%(For $\tan \beta < 5$, $\mu $ becomes  
%sensitive to $m_{H_d}^2$, 
%%and large $m_0$ gives negative     
%%contributions to $m_{H_u}^2$.  Both of these effects imply that, as
%and as $m_0$ increases $|\mu|$ also increases, and so there is no mixed   
%gaugino-Higgsino region for small $\tan \beta$.)
%%It was shown~\cite{feng} that for $\tan \beta \gsim 5$, the relic densities 
%%in the cosmologically interesting range over most of the focus
%%point regime with $m_0 > 1.5$ TeV. Even for $\tan \beta = 50$, 
%%$\Omega_{\tilde{\chi}_1^0} h^2$ never saturates the upper bound, 
%%even for $m_0 \sim 1 $ TeV.  As expalined above this additional suppression 
%%of $\Omega_{\tilde{\chi}_1^0} h^2$ id due to enhancing the process 
%%$\tilde{\chi}_1^0 \tilde{\chi}_1^0 \to A \to f \bar{f}$ since the coupling
%%the $Af\bar{f}$ coupling is proportional to $\tan\beta$ for isospin 
%%$-\frac{1}{2}$ fermions.
%However, as discussed in ref.\cite{focus}, one still needs large values for 
%$\tan \beta$ (of the order of 50) in order to have 
%$\sigma_{\tilde{\chi}_1^0-p} \lsim 
%10^{-6}$ pb. 
%%Moreover, the usual anti-correlation
%%between $\sigma_P$ and  $\Omega_{\tilde{\chi}_1^0} h^2$ also still holds in
%%this class of models. 

%\subsection{\normalsize Scenario with non-universal soft terms}

%The soft SUSY-breaking terms can have in general a
%non-universal structure in the MSSM. Such structure can
%be derived from SUGRA \cite{dilaton}. 
%For the case of the observable scalar masses,
%this is due to the non-universal couplings
%in the K\"ahler potential
%between the hidden sector fields breaking SUSY and the
%observable sector fields.
%For the case of the gaugino masses, this is due to the
%non-universality of the gauge kinetic functions associated to the
%different gauge groups.
%Explicit string constructions, whose low-energy limit is SUGRA,
%exhibit these properties \cite{dilaton}.
 
%It was shown recently, in the context of SUGRA, 
%that non-universality allows to increase \cite{Bottino,Arnowitt,Nath2}
%the neutralino-proton cross section for moderate values of $\tan\beta$.
%This can be carried out with non-universal 
%scalar masses
%and/or gaugino masses, 
%as we will discuss below.\\

%\hspace{-0.65cm}{\it $(i)$ Non-universal scalar masses}\\


%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%\begin{figure}[t]
%\begin{center}
%\epsfig{figure=arnow_m30-550.eps, 
%%width=7cm, 
%height=7cm}
%\end{center}

%\vspace{-0.5cm}

%\caption{
%The same as in Fig.~\ref{ellisfig}b
%%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ vs.
%%$m_{\tilde{\chi}_{1}^{0}}$ 
%but for $\tan{\beta}=10$ and using non-universal soft 
%scalar masses 
%as explained in the text.
%The universal case (green region) 
%is shown for comparison.
%}
%\label{arnowit}
%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%Non-universality in the Higgs sector, concerning dark matter, was studied in 
%refs.\cite{Ole,Fornengo,Bottino}. Subsequently, non-universality in
%the sfermion sector was added in the analysis \cite{arna,Arnowitt}.
%In order to avoid potential problems
%with flavour changing neutral currents, it was 
%assumed that
%the first two generations of squarks
%and sleptons have a common scalar mass
%$m_0$ at $M_{GUT}$, and 
%non-universalities were allowed in the third generation and
%Higgs sector.
%Thus the soft masses can be parameterized as follows:
%\begin{eqnarray}
%m_{H_{d}}^2&=&m_{0}^{2}(1+\delta_{1}), \quad m_{H_{u}}^{\ 2}=m_{0}^{2}
%(1+ \delta_{2}),\nonumber \\
%m_{Q_{L}}^2&=&m_{0}^{2}(1+\delta_{3}), \quad m_{u_{R}}^{\ 2}=m_{0}^{2}
%(1+\delta_{4}), \nonumber\\
%m_{e_{R}}^2&=&m_{0}^{2}(1+\delta_{5}),  \quad m_{d_{R}}^{\ 2}=m_{0}^{2}
%(1+\delta_{6}), \nonumber\\
%m_{L_{L}}^2&=&m_{0}^{2}(1+\delta_{7}),     
%\end{eqnarray}
%where 
%$Q_{L}=(\tilde{t}_{L}, \tilde{b}_{L})$, $L_{L}=(\tilde{\nu}_{L},
%\tilde{\tau}_{L})$, $u_{R}=\tilde{t}_{R}$, $e_{R}=\tilde{\tau}_{R}$, and 
%it is assumed that $ -1 \leq \delta_{i} \leq 1 $. 




%As explained at the beginning of this section~3,
%$\mu^{2}$ is one of the important parameters when
%computing
%the neutralino-nucleon cross section.
%Its value is determined by condition (\ref{electroweak}) and can
%be significantly reduced for some choices of $\delta$'s. We can have
%a qualitative
%understanding of the effects of the $\delta$'s on $\mu$ from
%the following.
%First, when $m_{H_u}^2$($m_{H_d}^2$) at $M_{GUT}$ increases(decreases)
%its negative(positive) contribution at low energy in eq.(\ref{electroweak})
%is less important. Second, when $m_{Q_{L}}^2$ and $m_{u_{R}}^2$
%at $M_{GUT}$ decrease, due to their contribution proportional
%to the top Yukawa coupling in the RGE of $m_{H_u}^2$ the negative
%contribution of the latter to $\mu^2$ is again less important.
%%The importance of including both effects was pointed out in
%%ref.\cite{Arnowitt}.
%%can be read from
%%the following analytic expression \cite{Arnowitt} for low and
%%intermediate $\tan\beta$:
%%
%%\begin{eqnarray}
%%\mu^{2} & = & \frac{t^{2}}{t^{2}-1} \left[ \left\{ \frac{1-3 D_{0}}{2} +
%%\frac{1}{t^{2}} \right\} + \left\{
%%\frac{1-D_{0}}{2}(\delta_{3}+\delta_{4})-\frac{1+D_{0}}{2} \delta_{2} +
%%\frac{\delta_{1}}{t^{2}} \right\} \right] m_{0}^{2} \nonumber \\ & & + 
%%\mbox{universal parts + loop corrections}       
%%\end{eqnarray}
%%
%%where $t \equiv \tan{\beta}$ and $D_{0} \cong 1 - 
%%(\frac{m_{t}}{200 \sin{\beta}})^{2}$. In general $D_{0}$ is small, $D_{0}
%%\leq 0.2$, and hence
%%the squark non-universality, $\delta_{3}$ and $\delta_{4}$, produce 
%%comparable size effects as the Higgs non-universalities $\delta_{1}$ and 
%%$\delta_{2}$, so that both must be included. 
%Thus one can deduce that 
%$\mu^2$ will be reduced (and hence $\sigma_{\tilde{\chi}_1^0-p}$ increased)
%by choosing $\delta_3, \delta_4, \delta_1 < 0$ and $\delta_2 >0$.




%Following this analysis \cite{Bottino,Arnowitt} we show in Fig.~\ref{arnowit},
%for $\tan\beta=10$,
%a scatter plot of
%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ as a function of $m_{\tilde{\chi}_{1}^{0}}$
%for a scanning of the parameters as follows:
%$0 \leq \delta_2 \leq 1$, $-1 \leq \delta_{1,3,4} \leq 0$.
%The other $\delta'$s are not so important in the computation and we take
%them vanishing.
%We are also taking $A=M_{1/2}$, 30 GeV $\leq m_0\leq 550 $ GeV as in
%Fig.~\ref{ellisfig}b,
%and we have to take now 140 GeV $\lsim M_{1/2} \lsim
%450$ GeV.
%For comparison we superimpose also the region (green area) 
%obtained in Fig.~\ref{ellisfig2} for $\tan\beta=10$
%with universality, $\delta_i=0$.
%We see that non-universal scalar masses can help in increasing the values of
%$\sigma_{\tilde{\chi}_{1}^{0}-p}$.
%%Note that the line associated to the 
%%universal case $\delta_i=0$ corresponds to the minimum value of 
%%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ (see also  Fig.~\ref{ellisfig}).
%In fact non-universality in the Higgs sector gives the most important
%effect, and including the one in the sfermion sector the cross
%section only increases slightly.
%Of course, as discussed in detail in Subsection 3.1, for
%larger values of $\tan{\beta}$ one can get 
%larger cross sections.\\

%\hspace{-0.65cm}{\it $(ii)$ Non-universal gaugino masses}\\



%The effects of the non-universality of gaugino masses on dark matter
%in SUGRA scenarios have been studied 
%in ref.\cite{Yamaguchi,Nath2,Nelson}.
%In particular, in ref.\cite{Nath2}, the authors analyze in detail 
%the neutralino-proton cross section in the case of
%$SU(5)$ unified models with interesting results, 
%finding that the cross sections 
%can increase. 

%Here we are interested in the case of the standard model gauge group
%in order to compare our results with both, the universal case discussed
%in Sections 2 and 3.1 and the case with non-universal scalar masses
%discussed above.
%Let us then parameterize the soft gaugino masses at $M_{GUT}$ as follows:
%%%
%%\begin{eqnarray}
%%M_{1}&=&M_{1/2}(1+\delta'_{1}), \quad M_2=M_{1/2}
%%(1+ \delta'_{2}),\nonumber \\
%%M_3&=&M_{1/2}(1+\delta'_{3}), \quad m_{u_{R}}^{\ 2}=m_{0}^{2}
%%(1+\delta_{4})\ ,     
%%\end{eqnarray}
%%
%\begin{eqnarray}
%M_{1}&=&M_{1/2}(1+\delta'_{1}), \quad M_2=M_{1/2}
%(1+ \delta'_{2}), \quad M_3=M_{1/2}(1+\delta'_{3})\ ,     
%\end{eqnarray}
%%
%where $M_{1,2,3}$ are the bino, wino and gluino masses, respectively, and
%we assume that $ -1 \leq \delta'_{i} \leq 1 $. 

%%Let us discuss now which values of the parameters are interesting
%%in order to increase the cross section, with respect to the
%%universal case $\delta'_i=0$.
%%As discussed in Section~2,
%%for
%%low or moderate $\tan\beta$ the lightest neutralino is mainly gaugino $P>0.9$,
%%and in particular bino since $N_{11}>>N_{12}$. However, relaxing the
%%universality condition for gaugino masses, $M_2<<M_1$
%%will produce the opposite situation $N_{11}<<N_{12}$, and therefore
%%the lightest neutralino will be mainly wino.
%%Since the wino component of the neutralino couples through $SU(2)$
%%interactions, unlike the bino component which couples through $U(1)$
%%ones, the cross section will increase (see eq. ????????????).

%%On the other hand, $M_3$ appears in the RGEs of squark masses, so e.g.
%%their contribution proportional
%%to the top Yukawa coupling in the RGE of $m_{H_u}^2$ will
%%do this less negative if $M_3$ is small. Therefore $\mu^2$ becomes smaller.

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%\begin{figure}[t]
%%\begin{center}
%%\epsfig{figure=nonunivg_m30-550.eps,width=9cm, height=6.5cm}
%%\end{center}
%%\caption{
%%The same as in Fig.~\ref{ellisfig}
%%but only for $\tan{\beta}=10$ and using non-universal soft 
%%gaugino masses 
%%as explained in the text. The line ????????corresponds to the
%%universal case.  
%%\label{nunivg.eps}}
%%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%%Taking into account both effects, 
%%we show in Fig.~\ref{nunivg.eps},
%%for $\tan\beta=10$,
%%a scatter plot of
%%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ as a function of $m_{\tilde{\chi}_{1}^{0}}$
%%for a scanning of the parameters,
%%$ -1 \leq \delta'_{1} \leq 1 $,
%%$ -1 \leq \delta'_{2} \leq 1 $,
%%$ -1 \leq \delta'_{3} \leq 0 $, imposing $M_3<M_{1,2}$.
%%We
%%fix 
%%$M_{1/2}= 225$ GeV.
%%As in the previous figures
%%we are 
%%taking 30 GeV $\leq m_0\leq 550$ GeV.
%%We also superimpose for comparison the region (green area) 
%%obtained in Fig.~\ref{ellisfig2} for $\tan\beta=10$
%%with universality, $\delta'_i=0$.
%%Clearly non-universal gaugino masses produce a large 
%%increment in the cross section.\\

%Let us discuss now which values of the parameters are interesting
%in order to increase the cross section, with respect to the
%universal case $\delta'_i=0$. In this sense, it is worth noticing that
%$M_3$ appears in the RGEs of squark masses, so e.g.
%their contribution proportional
%to the top Yukawa coupling in the RGE of $m_{H_u}^2$ will
%do this less negative if $M_3$ is small. Therefore $\mu^2$ becomes smaller.


%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%\begin{figure}[t]
%\begin{center}
%\epsfig{figure=nonunivg_m30-550.eps,
%%width=9cm, 
%height=7cm}
%\end{center}

%\vspace{-0.5cm}

%\caption{
%The same as in Fig.~\ref{ellisfig}b
%but only for $\tan{\beta}=10$ and using non-universal soft 
%gaugino masses 
%as explained in the text. The universal case (green region) 
%is shown for comparison.
%%corresponds to the
%%universal case.  
%\label{nunivg.eps}}
%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%Taking into account this effect, 
%we show in Fig.~\ref{nunivg.eps},
%for $\tan\beta=10$,
%a scatter plot of
%$\sigma_{\tilde{\chi}_{1}^{0}-p}$ as a function of $m_{\tilde{\chi}_{1}^{0}}$
%for the following scanning of the parameters:
%$ -1 \leq \delta'_{1,2} \leq 1 $
%%$ -1 \leq \delta'_{2} \leq 1 $
%and $ -2/3 \leq \delta'_{3} \leq 0 $ (where the lower bound
%is due to the experimental bound on gluino masses), imposing 
%$M_3<M_1, M_2$.
%We
%fix 
%$M_{1/2}= 225$ GeV and $A=M_{1}$.
%As in the previous figures
%we are 
%taking 30 GeV $\leq m_0\leq 550$ GeV.
%We also superimpose for comparison the region (green area) 
%obtained in Fig.~\ref{ellisfig2} for $\tan\beta=10$
%with universality, $\delta'_i=0$.
%Clearly non-universal gaugino masses produce a large 
%increment in the cross section.

%Let us finally remark that the upper and right hand side regions with
%large cross sections in the
%figure correspond to points of the parameter space fulfilling 
%$M_2<M_1$ (and $M_3$ close to its lower bound).
%As discussed in Section~2,
%for
%low or moderate $\tan\beta$ the lightest neutralino is mainly gaugino $P>0.9$,
%and in particular bino since $N_{11}\gg N_{12}$. However, relaxing the
%universality condition for gaugino masses, $M_2<M_1$
%will produce $N_{11}<N_{12}$, and therefore
%the lightest neutralino will have an important wino 
%component\footnote{It is worth noticing that this situation
%also arises in anomaly-mediated SUSY-breaking scenarios, where
%the cross section can also be increased \cite{anomaly,anomaly2}.}.
%Since the latter couples through $SU(2)$
%interactions, unlike the bino component which couples through $U(1)$
%ones, the cross section increases.\\
%% (see eq. ????????????).



%\hspace{-0.65cm}{\it $(iii)$ Non-universal gaugino and scalar masses}\\

%Given the above situation concerning the enhancement of
%neutralino-proton cross sections through non-universality 
%%the most simple way
%%to obtain $\sigma_{\tilde{\chi}_{1}^{0}-p}>10^{-6}$ pb
%for moderate $\tan\beta$, it is worth analyzing in
%principle the combination of both possibilities,
%non-universal gaugino and scalar masses.
%However 
%%Thus we show in Fig.~\ref{nunivgs} 
%the consequence
%for the cross section of combining the parameters studied in
%{\it (i)} and {\it (ii)} is not very different from the one obtained
%in Fig.~\ref{nunivg.eps}.
%We have explicitly checked that the qualitative pattern is basically
%the same. 
%%We find that in this class of scenarios, it is possible to enhance the 
%%neutralino-proton cross section 
%%and to obtain $\sigma_{\tilde{\chi}_{1}^{0}-p}$ 
%%within the experimental DAMA region with moderate $\tan \beta$. 




%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%\begin{figure}[t]
%%\begin{center}
%%\epsfig{figure=nonunivgs_m30-550.eps,
%%%width=9cm, 
%%height=7cm}
%%\end{center}
%%\caption{
%%The same as in Fig.~\ref{ellisfig}b
%%but only for $\tan{\beta}=10$ and using non-universal soft 
%%gaugino and scalar masses 
%%as explained in the text. The line ????????corresponds to the
%%universal case.  
%%\label{nunivgs}}
%%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%






%%=================================================
%%WRITTEN BY SHAABAN IN THE PREVIOUS VERSION

%%It was realized that the reason for the failure of low $\tan\beta$ mSUGRA
%%to solve the dark matter problem is the low annhiliation cross section 
%%for the neutralino. The only channel capable of providing a suitable 
%%cross section
%%is the t--channel sfermion exchange which is only effeicent in a small
%%region of parameter space. If we relax the GUT relationalship between the 
%%gaugino masses but still remain in the large $\vert \mu \vert$ limit 
%%(low $\tan \beta$) then we will continue to have a predominantly gaugino--like
%%LSP ($P \sim 1$) with the relative values of $N_{11}$ and $N_{12}$ governed
%%by the relative values of $M_1$ and $m_2$. Decreasing $M_2$ relative to $M_1$
%%at the electroweak scale increases the wino content of the LSP.
%%This also could help in enhancing the LSP--nucleon cross section.

%%Here, We consider as an example the following  non--universal soft breaking 
%%terms at $M_{GUT}$ where the gaugino masses are non--universal, namelly
%%we assumed that $M_2 < M_1 < M_3$ and the soft scalar masses for the first
%%and second generations are given by $m_{1,2}$ and for the third generation 
%%is given by $m_{3}$ where  
%%\begin{eqnarray}
%%&& m_{H_2}^2 = m_3^2 =  a~ m^2~,~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~a > 1
%%\;, 
%%\nonumber \\
%%&& m_{H_1}^2 = m_{l,2}^2  = b~ m^2 ~,~~~~~~~~~~~~~~~~~~~~~~~~~~~0 \leq b < 1
%%\;.
%%\label{mimi}
%%\end{eqnarray}
%%Since the smaller(bigger) $m_{H_1}^2$($m_{H_2}^2$) at $M_{GUT}$ is,
%%the less important the positive(negative) contribution
%%to $\mu$ at the electroweak scale becomes,
%%the above non-universality for Higgs masses will decrease the value of
%%$\mu$. Reducing the soft scalar masses for the first generation also 
%%help in enhancing the cross section. We have fixed $M_2$ such that the 
%%lightest chargino mass at the weak scale is of the order of 
%%the current experimental limit, i.e. $\mathcal{O}(100)$ GeV and assume that 
%%$M_1 = 2 M_2$ while $M_3 = \sqrt{3} m_0$. 
%%Finally we assume that the A-terms to be of order $-3 m_0$. 

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%\begin{figure}[ht]
%%\begin{center}
%%\epsfig{figure=nuniv.eps,width=13cm, height=5.5cm}
%%\end{center}
%%\caption{Values for $\sigma_{\tilde{\chi}_{1}^{0}-p}$ vs. 
%%$m_{\tilde{\chi}_1^0}$.  
%%\label{nuniv.eps}}
%%\end{figure}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

%%We find that in this class of models, it is possible to enhance the 
%%LSP--nucleon cross section and to obtain $\sigma_{\tilde{\chi}_{1}^{0}-p}$ 
%%within the experimental DAMA region with low $\tan \beta$. 


%%======================================================


%\subsection{\normalsize Scenario with intermediate unification scale}


The analyses of the neutralino-nucleon cross section in mSUGRA, 
mentioned above, were performed assuming the
unification scale
$M_{GUT} \approx 10^{16}$ GeV, as is usually done in the SUSY literature.
However, it was recently 
%realized that 
%the string scale may be anywhere between the weak and the Plank 
%scale \cite{Lykken}-\cite{weakandstronghete}.
%To use the value of the initial scale,
%say $M_I$, as a free parameter for the running of the soft terms
%is particularly interesting since 
%there are several arguments in favour of SUSY scenarios
%with scales 
%$M_I\approx 10^{10-14}$ GeV.
%First, these scales were suggested \cite{stronghete,typeIinter}
%to explain many experimental observations as
%neutrino masses or the scale for axion physics. 
%Second, with the string scale of the order of
%$10^{10-12}$ GeV
%one is able
%to attack the hierarchy problem of unified theories 
%without invoking any hierarchically suppressed non-perturbative
%effect \cite{stronghete,typeIinter}. Third,
%for intermediate scale scenarios
%charge and color breaking constraints,
%which are very strong with the usual scale $M_{GUT}$ \cite{servidor},
%become less important \cite{Allanach}.
%There are other arguments in favour 
%of scenarios with initial scales $M_I$ smaller
%than $M_{GUT}$.
%For example these scales
%might also
%explain the observed ultra-high energy ($\approx 10^{20}$ eV) cosmic rays
%as products of long-lived massive string mode 
%decays \cite{stronghete,typeIinter} (see ref.\cite{cosmic} for more
%details about this possibility). Besides,
%several models of chaotic inflation favour also these scales \cite{caos}.
%Inspired by these scenarios, 
pointed out \cite{muas} 
that this
%neutralino-proton 
cross section 
$\sigma_{\tilde{\chi}_1^0-p}$
is very sensitive to the variation of the initial scale 
for the running of the soft terms.
In particular, intermediate unification scales were considered.
For instance, by taking $M_I=10^{10-12}$ GeV rather than 
$M_{GUT}$, regions in the parameter space of mSUGRA have been 
found 
where  $\sigma_{\tilde{\chi}_1^0-p}$
is in the expected range of sensitivity of present detectors,
%DAMA \cite{experimento1} and CDMS \cite{experimento2} detectors, 
and this
even for moderate values of $\tan\beta$ ($\tan\beta\gsim 3$). 
This analysis 
was performed in the universal scenario for the soft terms. 
In contrast, in the usual case with initial scale at $M_{GUT}$,
this large cross section is achieved only for $\tan\beta \gsim 20$.


\begin{figure}[t]
\begin{center}
%\includegraphics[height=1.5in]{running2.eps}
\epsfig{file= running2.eps,width=7cm,height=3.5cm,angle=0}
\end{center}
\caption{
Running of the soft Higgs masses-squared with energy $Q$.}
\label{run}
\end{figure}





%\begin{figure}[t]
%\begin{center}
%\epsfig{file= p24f007.eps,width=5.75cm,height=4.5cm,angle=0}
%\hspace{0.5cm}\epsfig{file= p24f006.eps, width=5.75cm, height=4.5cm,angle=0}
%\end{center}

%\vspace{-0.5cm} 

%\caption{Running of the gauge couplings with energy, shown
%with solid lines, assuming
%(a) non universality and (b) universality of couplings at the
%initial scale $M_I$. 
%For comparison the usual running of the MSSM couplings
%is also shown with dashed lines.}
%\label{uni}
%\end{figure}




%Before trying to understand this result, let us discuss what we
%mean by an intermediate unification scale. 
%Concerning this point
%two possible scenarios
%are schematically shown in Fig.~\ref{uni} for the example
%$M_I= 10^{11}$ GeV. In scenario (a) 
%the gauge couplings are non universal,
%$\alpha_i\neq\alpha$, and their values
%depend on the initial scale $M_I$ chosen.
%An interesting proposal in order to obtain this scenario
%in the context of
%type I string models is the following. 
%If the standard model comes from the
%same collection of D-branes, 
%stringy corrections might change the boundary conditions at the string scale
%$M_I$ to mimic the effect of field theoretical logarithmic 
%running \cite{Rigolin,mirage}.
%Another possibility giving rise to a similar result
%may arise when
%the gauge groups came from different types of D-branes.
%Since different D-branes have associated different couplings,
%this implies the non universality of the gauge couplings. 
%We will discuss this possibility in some detail below.

%On the other hand, scenario (b) with gauge coupling 
%unification at $M_I$, $\alpha_i=\alpha$, can
%be obtained with 
%the addition of extra fields
%in the massless spectrum. For the example of the figure these are
%doublets and singlets under the standard model gauge group.


%As we will see below, the values of the gauge coupling constants at the
%intermediate
%scale will be important in the computation of the cross section, and
%scenario (a) will be more interesting than (b).


%To understand this result qualitatively, we show schematically in
%Fig.~\ref{run} 
%the well known evolution of $m_{H_d}^2$ and $m_{H_u}^2$ with the
%scale
%%\footnote{Let us remark that, given the convention used throughout
%%this review for gaugino masses in the Lagrangian, 
%%${\cal L} =\frac{1}{2}\sum_{a} M_a {\lambda}_a \lambda_a$ + h.c., we
%%are using the renormalization group equations (RGEs) obtained e.g.
%%in ref.\cite{rges}, but with an opposite sign in the
%%gaugino contributions to the RGE's of the $A_0$ parameters.}. 
%Since $m_{H_u}^2$ becomes large and negative (notice also
%that $m_{H_d}^2$, neglecting
%bottom and tau Yukawa couplings, becomes positive), $|\mu|$ due
%to relation (\ref{electroweak}) 
%becomes also large, in particular much larger than
%$M_1$ and $M_2$. Thus, as can be easily understood,
%%from 
%%eqs.(\ref{mass}) and (\ref{lneu}), 
%the lightest neutralino will be mainly gaugino, and in particular
%bino since at low energy $M_1\approx \frac{1}{2}M_2$.



The fact that smaller initial scales imply a larger neutralino-proton
cross section can be understood from the variation in the value of 
$\mu$ with $M_I$.
One observes that, for $\tan\beta$ fixed, the smaller the initial
scale for the running is, the smaller the numerator in the
first piece of eq.(\ref{electroweak}) becomes. 
This can be understood qualitatively from Fig.~\ref{run}, where
the well known evolution of $m_{H_d}^2$ and $m_{H_u}^2$ with the
scale is schematically shown. 
Clearly, the smaller the initial scale is, the shorter the
running becomes. As a consequence, 
also the less important the positive(negative) contribution 
$m_{H_d}^2$($m_{H_u}^2$) to $\mu$ in eq.(\ref{electroweak}) becomes.
Thus 
%The above conclusion has important consequences
%for the cross section.
%As is well known, and can easily be understood from the neutralino mass
%matrix in
%eq.(\ref{mass}), when 
$|\mu|$ decreases. 

Now, since 
${\cal L} \sim \mu \tilde{H}^0_u \tilde{H}^0_d$ + h.c.,
the Higgsino
components
of the lightest neutralino, $N_{13}$ and $N_{14}$ in eq.(\ref{lneu}),
increase.
In Fig.~\ref{N_1i}, for $\tan\beta=10$ and $m_0=150$ GeV, 
we exhibit the gaugino-Higgsino components-squared $N_{1i}^2$ 
of the lightest neutralino as a function of its mass $m_{\tilde{\chi}_1^0}$
for 
two different values of 
the initial scale, 
$M_I=10^{16}$ GeV  $\approx M_{GUT}$ and 
$M_I=10^{11}$ GeV. 
%This is to be compared with Fig.~\ref{ellisfig}
%where the initial scale is $M_{GUT}\approx 10^{16}$ GeV.
Clearly, the smaller the scale is, the larger 
the Higgsino components become. 
%In particular, for 
%$M_I=10^{16}$ GeV the lightest neutralino
%is mainly Bino since $N_{11}$ is extremely 
%large. The scattering channels through Higgs exchange are
%suppressed (recall that the Higgs-neutralino-neutralino couplings
%are proportional to $N_{13}$ and $N_{14}$) and therefore
%the cross section is small as we see explicitly in 
%Fig.~\ref{sigmaM_I}.
%As a matter of fact, the scattering channels through squark exchange
%are also suppressed by the mass of the first-family squarks.
%Indeed in this limit the cross section can be approximated as
%
%\bea
%\sigma_{\tilde\chi_1^0-p}
%\propto {m_r^2}\frac{\alpha^2}{\left(m_{\tilde s}^2-
%m_{\tilde{\chi}_1^0}\right)^2}  f_s^2   |N_{11}|^4
%\ .
%\label{cross}
%\eea
%
%where $m_r$ is the reduced mass and $m_{\tilde q}$, $\theta$
%are the mass and the mixing angle of the first-family squarks
%respectively.
%However, 
For
$M_I=10^{11}$ GeV, e.g. the Higgsino contribution $N_{13}$  
becomes important 
%in Fig.~\ref{N_1i} 
and even dominant for 
$m_{\tilde{\chi}_1^0}\lsim 140$ GeV.
Then, the scattering channels through Higgs exchange shown in 
Fig.~\ref{Feynman} are important,
%unlike the case with $M_I=10^{16}$ GeV where they are
%suppressed (recall that the Higgs-neutralino-neutralino
%couplings are proportional to $N_{13}$ and $N_{14}$), 
and therefore
the cross section may be large.
%As a matter of fact, the scattering channels through squark 
%exchange, shown also in Fig.~\ref{Feynman}, 
%are also suppressed by the mass of the squarks. Indeed
%in this limit the cross section (\ref{crosssection}) can be approximated as


\begin{figure}[ht]
\begin{center}
\epsfig{file= componentes.eps, 
height=7cm,angle=0}
\end{center}
\vspace{-0.5cm}
\caption{Gaugino-Higgsino components-squared
of the lightest neutralino as a function of its mass for
the unification scale, $M_I=10^{16}$ GeV, and for the intermediate scale,
$M_I=10^{11}$ GeV.
}
\label{N_1i}
\end{figure}



%with $\tan\beta=3$ and 
% (e.g. with $\tan\beta=3$ this is obtained for 
%$m_{\tilde{\chi}_1^0}\lsim 65$ GeV).
%Following the arguments in Section 3 this will imply larger cross sections.
%Indeed scattering channels through Higgs exchange are now important
%and their contributions 
%to cross sections can be schematically approximated as
%
%\bea
%\sigma_{\tilde\chi_1^0-p}
%\propto {m_r^2}
%\frac{\lambda_s^2 \alpha}{m_h^4}
%f_s   |N_{1i} N_{11}|^2 
%\ ,
%\label{cross2}
%\eea
%
%where $i=3,4$, $\lambda_s$ is the strange Yukawa coupling and
%$m_h$ represent the Higgs masses.
%For moderate values of 
%$\tan\beta$
%as 
%those analyzed here, the reason being 
%that the top(bottom) Yukawa coupling 
%decreases(increases) since it is proportional
%to $\frac{1}{\sin\beta}$($\frac{1}{\cos\beta}$).
%This implies that the negative(positive) contribution 
%$m_{H_u}^2$($m_{H_d}^2$) to $\mu^2$ in eq.(\ref{electroweak}) 
%is less important.
%The discussion of the cases with $\tan\beta>10$ is more subtle
%and will be carried out below. 

\newpage

This is shown in 
Fig.~\ref{sigmaM_I}, where
the cross section as a function
of the lightest neutralino mass $m_{\tilde{\chi}_1^0}$ is plotted.
In particular we are comparing the result for the scale $M_I=M_{GUT}$
%studied in Figs.~\ref{ellisfig} and \ref{ellisfig2} 
with the result for 
the intermediate scale $M_I=10^{11}$ GeV.
For instance, when $m_{\tilde{\chi}_1^0}=100$ GeV, 
$\sigma_{\tilde\chi_1^0-p}$ 
for $M_I=10^{11}$ GeV is two orders of magnitude larger
than for $M_{GUT}$.
In particular, for $\tan\beta=3$, one finds 
$\sigma_{\tilde\chi_1^0-p} \lsim 10^{-7}$ pb 
if the initial scale is $M_I=10^{16}$ GeV.
However $\sigma_{\tilde\chi_1^0-p} \lsim 10^{-6}$ GeV is possible if 
$M_I$ decreases. 
%For $M_I\lsim 10^{12}$ GeV,
%taking into account the experimental lower bound on the lightest
%chargino
%mass
%$m_{\tilde\chi_1^{\pm}}=90$ GeV, 
%the range 70 GeV $\lsim m_{\tilde{\chi}_1^0}\lsim$ 100 GeV is 
%even consistent with the DAMA limits.


%and therefore  
%the spin independent cross section also 
%increases \cite{muas}.
%This is shown  in Figs.~\ref{N_1i} and \ref{sigmaM_I}.
%In fact these figures correspond to the scenario 
%in Fig.~\ref{uni}a with non-universal gauge couplings.
%For the scenario in Fig.~\ref{uni}b, 
%only with $\tan\beta\gsim 20$ one obtains
%regions consistent with DAMA limits.
%One of the reasons being that now
%$\alpha_2 (M_I)$ and $\alpha_1 (M_I)$ are bigger than in scenario (a) 
%and therefore the low-energy bino and wino masses appearing
%in eq.(\ref{mass}) are smaller.
%As a consequence 
%%$|\mu|$ 
%the increment of the cross section is less important.


It is also worth noticing
that, for any fixed value of $M_I$, the larger
$\tan\beta$ is, the larger
the Higgsino contributions become,
%The discussion concerning this point in Subsection~3.1 for $M_{GUT}$ is also
%valid for any initial scale $M_I$.
%As mentioned before, the larger
%$\tan\beta$ is, the larger the Higgsino contributions become, 
and
therefore the cross section increases.
For $\tan\beta=10$ we see in Fig.~\ref{sigmaM_I}
that the range 70 GeV $\lsim m_{\tilde{\chi}_1^0}\lsim$ 100 GeV is now
consistent 
with DAMA limits. 

\begin{figure}[t]
\begin{center}
\epsfig{file= feynman.eps,height=3.5cm,angle=0}
\end{center}
\caption{Feynman diagrams contributing to neutralino-nucleon cross section.}
\label{Feynman}
\end{figure}

\begin{figure}[ht]
\begin{center}
\epsfig{file= intermediate.eps, 
height=7cm}
\end{center}
\vspace{-0.5cm}
\caption{Scatter plot of the neutralino-proton cross section
as a function of the neutralino mass for two values of the initial scale,
$M_I=10^{16}$ GeV and $10^{11}$ GeV, and for $\tan\beta=3$ and 10.
DAMA and CDMS current 
experimental limits and projected GENIUS limits are shown.
}
\label{sigmaM_I}
\end{figure}  
%



%This corresponds to $M_I\lsim 10^{14}$ GeV.
%For $\tan\beta=20$, although not shown in the figure,
%it is obtained that the above range 
%Finally, we show in Fig.~3 the case increases to 
%50 GeV $\lsim m_{\tilde{\chi}_1^0}\lsim$ 170 GeV, corresponding
%now to  $M_I\lsim 10^{16}$ GeV.




Let us remark that these figures have been obtained \cite{muas}
taking $30\lsim m_0\lsim 550$ GeV and $A_0=M_{1/2}$.
In any case, the cross section is 
not very sensitive to the specific values
of $A_0$. In particular it was checked that 
this is so for 
$\mid A_0/M_{1/2}\mid \lsim 1$.
%For example, relation $A_0=-M_{1/2}$ 
%is particularly interesting since it arises naturally
%in several string models \cite{dilaton,Rigolin}. 

%and\footnote{It is worth noticing however,
%that for $m_0$ in the range $50-100$ GeV the neutralino is not the
%LSP in the whole parameter space. In some regions the stau is the LSP.}
%50 GeV $\lsim m_0\lsim 250$ GeV.
%It was also checked that the results 
%are consistent with present 
%bounds coming from accelerators.
%These are
%LEP and Tevatron bounds on SUSY masses and 
%CLEO $b\to s\gamma$ branching ratio measurements.




%Let us finally recall that
%the above computations have been carried out for the case of
%universal soft terms. This is not only the most simple
%possibility in the framework of SUGRA, but  
%is also allowed in the context of superstring models. This is e.g.
%the case of the dilaton-dominated SUSY-breaking 
%scenario \cite{dilaton}
%or weakly and strongly coupled heterotic models with one K\"ahler 
%modulus \cite{softM}.
%In this sense the analysis of neutralino-nucleon
%cross sections of those models 
%is included in the above analyses. This is exactly true for
%$M_I=M_{GUT}$. For intermediate unification scale,
%note that we are assuming gaugino mass universality
%at the high energy scale, 
%although in this scenario gauge couplings do not unify. 
%This situation is in principle
%possible in generic supersymmetric models, however it is not so natural in
%supersymmetric models from supergravity 
%where gaugino masses and gauge couplings
%are related through the gauge kinetic function. 
%Since an explicit string construction with nonuniversal
%gauge couplings and gaugino masses will be analyzed in detail below,
%we have chosen to simplify the discussion here
%assuming gaugino mass universality.


Let us finally recall that
%Obviously, 
%following the discussion of Subsection~3.3,
non universality of the soft terms in 
addition to intermediate scales
may introduce more flexibility in the computation.
In particular, decreasing $|\mu|$
in order to obtain regions in the parameter space giving rise to  
cross sections compatible with the sensitivity
of current detectors, may be easier.

\section{\large Superstring scenarios}

In the above section the analyses were performed assuming intermediate
unification scales.
In fact, this situation can be inspired by superstring theories, since
it was recently 
realized that 
the string scale may be anywhere between the weak and the Plank 
scale \cite{Lykken}-\cite{weakandstronghete}. 
For example, embedding the standard model inside D3-branes in type I
strings, the string scale is given by:
%
\bea
M_I^4= \frac{\alpha M_{Planck}}{\sqrt 2} M_c^3\ ,
\label{gravitino2}
\eea
%
where $\alpha$ is the gauge coupling and $M_c$ is the compactification scale. 
Thus one gets $M_I\approx 10^{10-12}$ GeV with $M_c\approx 10^{8-10}$ GeV.

Then, to use the value of the initial scale,
say $M_I$, as a free parameter for the running of the soft terms
is particularly interesting.
In addition, 
there are several arguments in favour of SUSY scenarios
with scales 
$M_I\approx 10^{10-14}$ GeV.
These scales were suggested \cite{stronghete,typeIinter}
to explain many experimental observations as
neutrino masses or the scale for axion physics. 
With the string scale of the order of
$10^{10-12}$ GeV
one is also able
to attack the hierarchy problem of unified theories 
without invoking any hierarchically suppressed non-perturbative
effect \cite{stronghete,typeIinter}. 
In supergravity models supersymmetry can be spontaneously broken in a 
hidden sector of the theory and the gravitino mass,
which sets the overall scale of the soft terms, is given by
%%
%\bea
%m_{3/2}\approx \frac{F}{M_{Planck}}\ ,
%\label{gravitino}
%\eea
%%
$m_{3/2}\approx \frac{F}{M_{Planck}}$,
where $F$ is the auxiliary field whose vacuum expectation value
breaks supersymmetry. 
Since in supergravity one would expect $F\approx M_{Planck}^2$, one  
obtains
$m_{3/2}\approx M_{Planck}$ and therefore 
the hierarchy problem solved in principle by supersymmetry
would be re-introduced.
However, if the scale
of the fundamental theory is $M_I\approx 10^{10-12}$ GeV instead of
$M_{Planck}$,
then $F\approx M_I^2$
and one gets $m_{3/2}\approx M_W$ in a natural way.

There are other arguments in favour 
of scenarios with initial scales $M_I$ smaller than $M_{GUT}$.
For example,
charge and color breaking constraints,
which are very strong with the usual scale $M_{GUT}$ \cite{servidor},
become less important \cite{Allanach}.
These scales might also
explain the observed ultra-high energy ($\approx 10^{20}$ eV) cosmic rays
as products of long-lived massive string mode decays.
\cite{stronghete,typeIinter} (see ref.\cite{cosmic} for more
details about this possibility). Besides,
several models of chaotic inflation favour also these scales \cite{caos}.

%
\begin{figure}[ht]
\begin{center}
\begin{tabular}{c}
\epsfig{file= branes.eps, width=9cm}\\
%\epsfig{file= p24f006.eps,width=10cm,height=7.0cm}
\end{tabular}
\end{center} 
\caption{A generic D-brane scenario giving rise to the gauge bosons
and matter of the standard model. It contains three D$p_3$-branes,
two D$p_2$-branes and one D$p_1$-brane, where $p_N$ may be
either 9 and $5_i$ or 3 and $7_i$. The presence of extra D-branes,
say D$q$-branes, is also
necessary. For each set the D$p_N$-branes
are in fact on the top of each other.} 
\label{branas}
\end{figure}
%


D-brane constructions are explicit scenarios where the two situations 
mentioned above, namely,
non-universality and intermediate scales, may occur.
Let us then analyse this possibility.

\subsection{\large D-branes}





The first attempts to study dark matter within these constructions
were carried out in scenarios with the unification scale  
$M_{GUT} \approx 10^{16}$ GeV
as the initial scale \cite{khalil,Nath2,Arnowitt2}
and dilaton-dominated SUSY-breaking scenarios 
with an intermediate scale as the initial scale \cite{bailin}.
However,
the important issue of the D-brane origin of the $U(1)_Y$ gauge group
as a combination of other $U(1)$'s 
and its influence on the matter distribution in these scenarios
was not included in the above analyses.
When this is taken into account, interesting results are 
obtained \cite{nosotros}. In particular, 
scenarios with the gauge group and particle content of the
SUSY standard model lead naturally to intermediate values for the
string
scale, in order to reproduce the value of gauge couplings
deduced from experiments. In addition, the soft terms 
turn out to be generically non universal.
Due to these results, 
large cross sections
in the small $\tan\beta$ regime
can be obtained.


Let us consider for example a type I string scenario \cite{nosotros}
where the gauge group 
$U(3)\times U(2)\times U(1)$, giving rise to
$SU(3)\times SU(2)\times U(1)^3$, arises
from three different types of D-branes, 
as shown schematically in Fig.~\ref{branas}.
For the sake of visualization each set is
depicted at parallel locations, but in fact they are intersecting each
other.
%and therefore
%the gauge couplings are
%non-universal
%as in Fig.~\ref{uni}a\footnote{To be precise, the running of the 
%$U(1)_Y$ gauge coupling is not exactly like in the figure since, due to the
%D-brane origin of the $U(1)$ gauge groups, relation (\ref{couplings})
%must be fulfilled. See in this respect Fig.~2 in ref.\cite{nosotros}.}.
Other examples with the standard model gauge group embedded in D-branes in 
a different way can be found in ref.\cite{nosotros}.
Here
$U(1)_Y$ is a linear combination
of the three $U(1)$ gauge groups arising from $U(3)$, $U(2)$ and
$U(1)$ within the three different D-branes. 
%
\begin{figure}[t]
\begin{center}
\begin{tabular}{c}
\epsfig{file= rgesinter.eps, width=6cm}\\
%\epsfig{file= p24f006.eps,width=10cm,height=7.0cm}
\end{tabular}
\end{center} 
\caption{Running of the gauge couplings of the MSSM with energy $Q$ 
embedding the gauge groups within different sets of D$p$-branes (solid lines).
Due to the D-brane origin of the $U(1)$ gauge groups, relation
(\ref{couplings}) must be fulfilled. 
For comparison
the running of the MSSM couplings with
the usual normalization factor for the hypercharge, $3/5$,
is also shown with dashed lines.} 
\label{corriendo}
\end{figure}
%
This implies
%
\bea
Y=-\frac{1}{3} Q_3 - \frac{1}{2} Q_2+ Q_1\ ,
\label{hypercharge}
\eea
%
and therefore, 
%
\begin{equation}
\frac{1}{\alpha_Y(M_I)} =     
\frac{2}{\alpha_1(M_I)} + \frac{1}{\alpha_2(M_I)} 
+ \frac{2}{3 \alpha_3(M_I)}\ ,
\label{couplings}
\end{equation}
%
where $\alpha_k$ correspond to the gauge couplings of the $U(k)$
branes.
Let us remark that since the D-branes are of different types,
the gauge couplings are
non-universal.
Now, using the RGEs for gauge couplings one obtains
%
\bea
\ln\frac{M_I}{M_s}=
\frac{2\pi\left(\frac{1}{\alpha_Y (M_Z)}-\frac{2}{\alpha_1 (M_I)}-
\frac{1}{\alpha_2 (M_Z)}-
\frac{2}{3\alpha_3 (M_Z)}\right)
+\left(b_Y^{ns}-b_2^{ns}-\frac{2}{3} b_3^{ns}\right)
\ln\frac{M_s}{M_Z}
}
{\left(\frac{2}{3} b_3^s + b_2^s -b_Y^s\right)}
\ ,
\label{MI}
\eea
%
where $b_j^s$ ($b_j^{ns}$) with $j=2,3,Y$ are the coefficients of 
the supersymmetric (non-supersym\-metric) $\beta$-functions, and 
the scale $M_{s}$ corresponds to the supersymmetric threshold, 
200 GeV $\lsim M_s\lsim$ 1000 GeV. 
For example, choosing the value of the coupling associated 
to the D$p_1$-brane in the range $0.07\lsim\alpha_1 (M_I)\lsim 0.1$,
and the experimental values for $\alpha_{3,2,Y}$,
one obtains
$M_I\approx 10^{10-12}$ GeV. This scenario is shown in Fig.~\ref{corriendo}
for $\alpha_1 (M_I)=0.1$ and $M_s=1$ TeV.
%
%As shown in ref.\cite{nosotros},  $\alpha_1(M_I) = 0.1$ leads
%to the string scale $M_I = 10^{12}$ GeV. 
%On the other hand,
Let us remark that 
the extra $U(1)$'s are anomalous and therefore the associated gauge
bosons
have masses of the order of $M_I$.

  
The analysis of the soft terms has been done under
the assumption that only the
dilaton ($S$) and moduli ($T_i$) fields contribute to SUSY
breaking and it has been found  that these soft terms  are generically
non-universal.
Using the standard parameterization \cite{dilaton} 
\begin{eqnarray}
&& F^S= \sqrt{3} (S+S^*) m_{3/2} \sin \theta\;, \nonumber \\
&& F^i= \sqrt{3} (T_i+T^*_i) m_{3/2} \cos \theta\; \Theta_i\;,
\end{eqnarray}
where
$i=1,2,3$ labels the three complex compact dimensions, and
the angle $\theta$ and the $\Theta_i$ with $\sum_{i} |\Theta_i|^2=1$,
just parameterize the direction of the goldstino in the $S$, $T_i$ field
space, one is able to obtain the following soft terms \cite{nosotros}.
The gaugino masses associated to the three gauge groups of the
standard model are given by
%\footnote{
%Note that the negative signs correspond to the convention used
%in this review for gaugino masses in the Lagrangian 
%as discussed in 
%footnote {\it b}. It is opposite to the one used in ref.\cite{nosotros} 
%where ${\cal L} =\frac{1}{2}\sum_{a=1,2,3} M_a \bar{\lambda}_a \lambda_a$.}
%
\bea
M_3 & = & \sqrt{3} m_{3/2} \sin \theta \ , \nn\\
M_{2} & = & \sqrt{3}  m_{3/2}\ \Theta_1 \cos \theta  \ , \nn\\
M_{Y} & = &  \sqrt{3}  m_{3/2}\ \alpha_Y (M_I)
\left(\frac{2\ \Theta_3 \cos \theta}{\alpha_1 (M_I)}
+\frac{\Theta_1 \cos \theta}{\alpha_2 (M_I)}
+\frac{2\ \sin \theta}{3 \alpha_3 (M_I)}
\right)\ .
\label{gaugino1}
\eea
%
The soft scalar masses of the three families are given by
%
\begin{eqnarray}
m^2_{Q_L} & = & m_{3/2}^2\left[1 -
\frac{3}{2}  \left(1 - \Theta_{1}^2 \right)
\cos^2 \theta \right] \ , \nn \\
m^2_{d_R} & = & m_{3/2}^2\left[1 -
\frac{3}{2}  \left(1 - \Theta_{2}^2 \right)   
\cos^2 \theta \right] \ , \nn \\
m^2_{u_R} & = & m_{3/2}^2\left[1 -
\frac{3}{2}  \left(1 - \Theta_{3}^2 \right)
\cos^2 \theta \right] \ , \nn \\
m^2_{e_R} & = & m_{3/2}^2\left[1- \frac{3}{2}
\left(\sin^2\theta + \Theta_{1}^2 \cos^2\theta  \right)\right] \ , \nn \\
m^2_{L_L} & = & m_{3/2}^2\left[1- \frac{3}{2}
\left(\sin^2\theta + \Theta_{3}^2 \cos^2\theta  \right)\right] \ , \nn \\
m^2_{H_u} & = & m_{3/2}^2\left[1- \frac{3}{2}
\left(\sin^2\theta + \Theta_{2}^2 \cos^2\theta  \right)\right] \ , \nn \\
m^2_{H_d} & = & m^2_{L_L} \;,     
\label{scalars1}
\end{eqnarray}
%
where e.g. $u_R$ denotes the three family squarks $\tilde{u}_R$, 
$\tilde{c}_R$, $\tilde{t}_R$.
Finally the trilinear parameters of the three families are
\begin{eqnarray}
A_{u} & = &  \frac{\sqrt 3}{2}m_{3/2}
   \left[\left(\Theta_{2} - \Theta_1
 - \Theta _{3}  \right) \cos\theta
- \sin\theta \; \right] \ ,
%\label{trintrin}
\nn \\
A_{d} & = &  \frac{\sqrt 3}{2}m_{3/2}
   \left[\left(\Theta_{3} - \Theta_1
  - \Theta _{2}  \right) \cos\theta
- \sin\theta \; \right] \ ,
%\label{trintrintrin}
\nn \\
A_{e} & = &  0\; .
\label{trilin11}
\end{eqnarray}
%


%
\begin{figure}[t]
\begin{center}
%\begin{tabular}{c}
\epsfig{file= casei1e12.eps, 
height=7cm
%width=13cm
}
\end{center}
\vspace{-1cm}
\caption{The same as in Fig.~\ref{sigmaM_I} but for 
%Scatter plot of the neutralino-proton cross section
%as a function of the neutralino mass for 
the D-brane scenario with 
the string scale $M_I=10^{12}$ GeV
discussed
in the text, and for $\tan\beta= 10$ and 15.}
%The string scale is $M_I=10^{12}$ GeV.
%DAMA and CDMS current limits
%and projected GENIUS limits are shown.}
\label{dbrane}
\end{figure}
%


Although these formulas for
the soft terms imply that one has in principle
five free parameters, $m_{3/2}$, $\theta$ and  $\Theta_i$ with $i=1,2,3$,
due to relation $\sum_i |\Theta_i|^2=1$ only four of them are
independent.
In the analysis the parameters $\theta$ and $\Theta_i$
are varied in the whole allowed range, $0\leq \theta\leq 2\pi$,
$-1\leq\Theta_i\leq 1$. For 
the gravitino mass, 
$m_{3/2}\leq 300$ GeV is taken.
Concerning Yukawa couplings, their values are fixed imposing 
the correct fermion mass spectrum at low energies, i.e.,
one is assuming that Yukawa structures of D-brane scenarios
give rise to those values.




Fig.~\ref{dbrane} displays a scatter plot of 
$\sigma_{\tilde\chi_1^0-p}$ as a function of the
neutralino mass $m_{\tilde\chi_1^0}$ for a scanning of the parameter space
discussed above. 
Two different values of $\tan\beta$, 10 and 15, are shown.
%LEP and Tevatron bounds
%on SUSY masses are included as in the previous sections. 
%They forbid e.g. values of
%$m_{3/2}$ smaller than 170 GeV.
%Although bounds coming from CLEO $b\rightarrow s\gamma$ branching
%ratio measurements are not included in the figures, one can check
%explicitly that their qualitative patterns are not modified.
It is worth noticing that
for $\tan\beta =10$ there are regions of the parameter
space consistent with DAMA limits.
In fact, one can check that $\tan\beta > 5$ is enough to
obtain compatibility with DAMA.
Since the larger $\tan\beta$ is, the
larger the cross section becomes, for $\tan\beta =15$ these regions
increase.

%Let us recall that both plots in the figure are obtained taking
%$m_{3/2}\leq 300$ GeV, which corresponds to squark masses 
%smaller than $500$ GeV  at low energies.
%Larger values of $m_{3/2}$ will always produce cross sections 
%below DAMA limits. In particular, 
%the right hand side and bottom of the plots will also be filled
%with points.
%Cross sections below
%projected GENIUS limits will be possible for both figures.
%On the other hand, it is worth mentioning that the isolated 
%points in the plots with, in general, very large values of the cross section
%correspond to values of the lightest stop mass extremely close to the
%mass of the LSP, 
%in particular $(m_{\tilde t}-m_{\tilde\chi_1^0})/m_{\tilde t}<0.01$.



%Finally, let us mention that scenarios where all gauge groups of the 
%standard model are
%embedded
%within the same set of D-branes, and therefore with gauge coupling
%unification, are also possible.
%However, unlike the previous scenario, 
%now $\tan\beta > 20$ is necessary in order to obtain regions
%consistent with DAMA limits \cite{nosotros}.
%As discussed above in the context of mSUGRA 
%this is due to the different values of the $\alpha$'s at the string scale  
%in both types of scenarios. 
%%Unlike the previous one where
%%there is no gauge coupling unification, here gauge couplings are unified.


%\newpage

\section{\large Relic neutralino density versus cross section}

As discussed in the Introduction, current dark matter detectors
are sensitive to a neutralino-proton cross section around $10^{-6}$ pb.
This value is obtained taking into account, basically, that the
density of dark matter in our Galaxy, which follows from the 
observed rotation curves, is 
$\rho_{DM}\approx 0.3$ GeV/cm$^3$.
Thus in this work we were mainly interested in reviewing the
possibility of obtaining such large cross sections in the
context of mSUGRA and superstring
scenarios. In order to compute the cross section
only simple field theory techniques are needed,
no cosmological assumptions about the
early Universe need to be used.

On the other hand, such
cosmological assumptions indeed must be taken into account 
when computing the amount of relic neutralino density
arising from the above scenarios.
Generically, through thermal production of neutralinos, one obtains \cite{kami}
%%
%\begin{equation}
%\Omega_{\tilde{\chi}_1^0} h^2\propto 1/ \langle 
%\sigma_{\tilde{\chi}_1^0}^{ann}\rangle
%\ ,
%\label{couplings}
%\label{assumption}
%\end{equation}
%%
%
\begin{equation}
\Omega_{\tilde{\chi}_1^0} h^2 \simeq \frac{C}
{<\sigma_{\tilde{\chi}_1^0}^{ann}. v>}
\ ,
\label{assumption}
\end{equation}
%
where $\sigma_{\tilde{\chi}_1^0}^{ann}$ is the  
cross section for annihilation of a pair of neutralinos
into standard model particles, $v$ is the 
relative velocity between the two neutralinos, 
and $<..>$ denotes thermal averaging.
The constant $C$ involves factors of Newton's constant, the temperature of the 
cosmic background radiation, etc. 
%where $\sigma_{\tilde{\chi}_1^0}^{ann}$ 
%is the cross section for annihilation of neutralinos.
Then one may compare this result with dark matter observations
in the Universe.
Let us then discuss briefly the effect of relic neutralino 
density bounds on cross sections.

The most robust evidence for the existence of dark matter comes from 
relatively small scales, in particular,
from the flat rotation curves of spiral Galaxies. 
%\cite{kami,salucci} are 
%$\Omega_{halo}\gsim 10\ \Omega_{vis}$ or 
%$\Omega_{DM}\ h^2\gsim 0.01-0.05$, where
%$h$ is the reduced Hubble constant. 
On the opposite side, observations at large scales,
%$(6-20)\ h^{-1} $ Mpc, 
have also provided 
estimates 
%\cite{freedman} 
of $\Omega_{DM}$.
% h^2\approx 0.1-0.6$, but values as low as 
%$\Omega_{DM} h^2\approx 0.02$ have also been quoted \cite{kaiser}.
Taking 
both kind of observations
%up-to-date limits on $h$, the 
%baryon density from nucleosynthesis and overall matter-balance   
one is able to obtain a favoured 
range \cite{contemporary}
%\cite{Sadoulet,primack00,NEW},
$0.1\lsim \Omega_{DM} h^2 \lsim 0.3$,
where $h$ is the reduced Hubble constant. 
% (at $\sim 2\sigma$ CL).
%Note that  conservative 
%lower limits in the small and large scales are 
%of the same order of magnitude.
It is worth noticing, however, that more conservative
lower limits have also been quoted in the literature (a
brief discussion can be found in ref.\cite{darkcairo} and references therein).

%The expected WIMP cosmological 
%relic density can be computed according to well 
%known techniques (see ref.\cite{kami}). 
%The general behaviour is  
%$\Omega_{\mbox{\tiny WIMP}} h^2\propto 1/ \langle 
%\sigma_{\mbox{\tiny WIMP}}^{ann}\rangle$,
%where $\sigma_{\mbox{\tiny WIMP}}^{ann}$ 
%is the cross section for annihilation of 
%WIMPs.
As is well known, for $\sigma_{\tilde{\chi}_1^0}^{ann}$ 
of the order 
of a weak-process cross section, $\Omega_{\tilde{\chi}_1^0}$ obtained
from eq.(\ref{assumption}) is 
within the favoured range discussed
above \cite{kami}. 
This is precisely the generic case when the lightest neutralino
is mainly bino. Then, the neutralino-nucleus cross section is
of the order of 1 pb,
i.e. $\sigma_{\tilde{\chi}_1^0-p}\approx 10^{-8}$ pb, 
and therefore it is natural to obtain
that neutralinos annihilate with very roughly
the weak interaction strength. 
%These cross sections were
%discussed in Section 2 where
%low and moderate values of $\tan\beta$ within mSUGRA were considered.
In fact, for these cross sections, there is always
a set of parameters which yield $0.1<\Omega_{\tilde\chi_1^0}h^2<0.3$.
This analysis, including a complete treatment of coannihilations
was carried out in refs.\cite{Ellis,Ellisco}.

On the other hand, in these proceedings we were interested in larger
neutralino-nucleon cross sections in order to be in the range
of sensitivity of current dark matter detectors.
It is then expected that such high neutralino-proton cross sections
$\sigma_{\tilde\chi_1^0-p}\approx 10^{-6}$ pb,
as those presented in Sections~2 and 3, will correspond to relatively low
relic neutralino densities.
This is in fact the general situation 
\cite{muas,bailin,nosotros}.
%-\cite{nosotros}

Let us remark, however,
that thermal production of neutralinos is not the only possibility,
moduli decays can also produce neutralinos.
Since the decay width of the moduli is
$\Gamma_{\phi}\sim \frac{m_{\phi}^3}{M^2}$, 
scenarios with intermediate scales 
might give rise to cosmological
results different from the usual ones 
summarized in eq.(\ref{assumption}).
Note that if $M=M_I$ the usual moduli problem 
may be avoided since a reheating temperature $T_{RH}$ small but 
larger than 1 MeV
can be obtained.
This is e.g. the case of the twisted moduli fields 
$M_{\alpha}$ in type I strings.
Recall that
$n/s
%\ h^2
\propto 1/T$
and since we can have a situation with 
$T_{RH}<<T_f\approx m_{\chi}/20\sim \cal{O}$(1 GeV), 
the relic neutralino density might  be larger than in the
usual case of thermal production. As a consequence,
$\Omega_{\tilde\chi_1^0}h^2> 0.1$ may be obtained \cite{preparation}.











%There is always a set
%of parameters for which the value of the relic density
%is still inside the ranges we considered above when discussing the
%observational bounds, but it is generically close to the
%conservative lower bound.
%The analysis of the relic neutralino density for
%scenarios with large $\tan\beta$ and non-universal scalar masses 
%was carried out in refs.\cite{Bottino,Arnowitt,Mario,Arnowittco}.
%Scenarios with non-universal gaugino masses were studied in
%%ref.\cite{Nath2} (see also \cite{Yamaguchi,Nelson}).
%refs.\cite{Yamaguchi,Nelson}.
%An analysis of the relic density for focus point supersymmetry 
%can be found in ref.\cite{focus}. 
%Discussions for
%scenarios with intermediate unification scales can be found in
%refs.\cite{muas}-\cite{nosotros}\footnote{Let us remark, however,
%that scenarios with intermediate scales might give rise to cosmological
%results different from the usual ones 
%summarized in eq.(\ref{assumption}) \cite{preparation}.}. 
%Examples in other scenarios of this possibility 
%can be found in refs.\cite{anomaly,kolb}.}.

%Finally, in case of 
%preferring the stronger lower bound
%$\Omega_{DM}h^2>0.1$, let us mention
%the possibility that not all the dark matter
%in our Galaxy are neutralinos. Then 
%$\Omega_{\tilde\chi_1^0}<\Omega_{DM}$,
%and therefore $\Omega_{\tilde\chi_1^0}<0.1$ is possible. However,
%due to the corresponding reduction in the density of neutralinos in the 
%Galactic halo, the neutralino-proton
%cross section should be increased in order to maintain the 
%experimental detection rates \cite{Ellis,elotrodeellis,Nojiri}.







%===============================================


% The relic density of WIMPs is 
%approximately given by 
%
%$$ \Omega_{\chi} h^2 \simeq \frac{C}
%{<\sigma_{ann}^{\chi}. v>}~ ,$$
%
%where $\sigma_{ann}^{\chi}$ is the total 
%annihilation cross section of WIMP pair into SM particles, $v$ is the 
%relative velocity between the two WIMPs, and $<..>$ denotes thermal averaging.
%The costant $C$ involves factors of Newton's costant, the temperature of the 
%cosmic background radiation, etc. 
%If the annihilation cross section is of order of weak scattering cross 
%sections the value of $\Omega_{\chi}h^2$ comes out in the desired range 
%(of order 0.2). In the presence of non--zero cosmological constant, the relic
%neutralino density lies in the range $0.1 \lsim \Omega_{\tilde{\chi}^0_1} 
%h^2 \lsim 0.3$ prefered by the large scale structure formation. However, it 
%is possible that there is more than one component in the cold dark matter, 
%for example axions, so that  $\Omega_{\tilde{\chi}^0_1}h^2 < 0.1$. In general 
%a decrease of $\Omega$ is associated with larger $\tilde{\chi}_1^0$ 
%annihilation cross sections, and hence larger elastic scattering cross 
%sections. However, the detection rate also must be reduced because of the 
%corresponding reduction in the density of LSPs in the Galactic halo. 
%Here we neglect this possibility and assume that all the cold dark matter 
%is composed of LSPs, so that $\Omega_{\tilde{\chi}^0_1}h^2 > 0.1$. 

%Since WIMPs annihilate with very roughly weak interaction strength, it is 
%natural to assume that their interaction with normal matter is also 
%approximately of this strength. This raises the hope of detecting relic 
%WIMPs directly, by observing their scattering off nuclei in a detector.


%==========================


%Given the partcile spectrum we can compute the thermal relic LSP density.
%This computation includes all the annihilation processes \cite{drees} which
%are used to compute a thermally averaged cross section $\langle \sigma v 
%\rangle_{ann}$ and freeze out temperature $x_{F} = T_F/m_{\tilde{\chi}_1^0}$.
%>From knowledge of the mass of the lightest neutralino $m_{\tilde{\chi}_1^0}$,
%$\langle \sigma v \rangle_{ann}$ and $T_F$, a relic aboundance can be 
%computed using the standard approximation~\cite{griest}
%\begin{equation}
%\Omega_{\tilde{\chi}_1^0} h^2 = \frac{1.07 \times 10^9~x_F}
%{g_*^{1/2} M_{p} (a_{\mathrm{eff}} + 3(b_{\mathrm{eff}} - 
%a_{\mathrm{eff}}/4)/x_F)} \mathrm{GeV}^{-1},
%\end{equation}
%where we have expressed the thermally averaged annihilation cross section
%as as expansion in powers of the relative velocity:
%\begin{equation}
%\langle \sigma v \rangle_{ann} = a_{\mathrm{eff}} + b_{\mathrm{eff}} v^2 +..
%\end{equation}

%A bino--like LSP annhilate predominantly through the exchange of a sfermion
%(especially, the exchange of $SU(2)$ singlet sleptons which, in many models,
%has small mass) in the $t$-- or $u$--channel. This yields interesting relic 
%densities for very reasonable choice of parameters. A wino--like LSP leads to 
%a very small relic density~\cite{yamaguchi} unless the LSP mass exceeds 1 TeV.
%In this case the mass splitting to the lightest chargino often only amounts 
%to a few hundred MeV, thus `co--annihilation' between LSPs and lightest
%charginos occurs, which greatly reduces the final LSP relic denisty. For the 
%higgsino--like LSP, the situation is more complicated. In this senario, the 
%$\tilde{\chi}_1^0 f \tilde{f}$ couplings are now Yukawa couplings, sfermion
%exchange contributions are small for LSPs that are too light to annihilate 
%into $t\bar{t}$ pairs. The annihialtion cross section for light 
%higgsino--like LSP is therefore small. Furthermore, if we consider the 
%co-annihilation between LSPs and next lightest neutralino and/or charginos 
%then the relic density turns out to be quite small. A higgsino--like LSP 
%with mass $\ge M_W$ has very large annihilation cross section into $W$ and 
%$Z$ pairs even in the absence of co-annihilation. 

\section{\large Final comments and outlook}

In the present proceedings we have studied  the direct detection of 
supersymmetric dark matter in the light of recent experimental efforts.
In particular, DAMA collaboration using a NaI detector
has reported recently 
%\cite{experimento1}
data favouring the existence of a WIMP signal in their search for
annual modulation. They require a large cross section of the order of
$10^{-6}$ pb. 
We have observed that there are regions in the parameter space
of mSUGRA scenarios with intermediate scales and
superstring scenarios with D-branes 
%\cite{Bottino}-\cite{nosotros} 
where such a value can be obtained, although it is fair to say that
smaller values
can also be obtained and even more easily.
The latter result may be important since 
CDMS collaboration using a germanium detector
has reported a null result for part of the region explored by DAMA. 
Clearly, more sensitive detectors
producing further data are needed to solve this contradiction.
Fortunately, many dark matter detectors are being projected.
This is the case e.g. of DAMA 250 kg., CDMS Soudan, GENIUS, etc.
%\cite{GENIUS}
where values of the cross section as low as 
$10^{-9}$ pb will be accesible. 

In summary, underground physics as the one discussed here in order
to detect dark matter is crucial. Even if neutralinos are discovered
at future particle accelerators such as LHC, only their direct detection
due to their presence in our galactic halo will confirm that they
are the sought-after dark matter of the Universe.


\Acknowledgements
%\noindent {\bf Acknowledgments}

\noindent
We thank E. Gabrielli and E. Torrente-Lujan
as co-authors of some of the works reported in
this review. D.G. Cerde\~no acknowledges the financial support
of the Comunidad de Madrid through a FPI grant.
The work of S. Khalil was supported by PPARC.
The work of C. Mu\~noz was supported in part by the Ministerio de 
Ciencia y Tecnolog\'{\i}a (Spain), and the European Union under contract 
HPRN-CT-2000-00148. 

%\newpage

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\end{document}

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