Dark Energy and Dark Matter

Abstract

It is a puzzle why the densities of dark matter and dark energy are nearly equal today when they scale so differently during the expansion of the universe. This conundrum may be solved if there is a coupling between the two dark sectors. In this paper we assume that dark matter is made of cold relics with masses depending exponentially on the scalar field associated to dark energy. Since the dynamics of the system is dominated by an attractor solution, the dark matter particle mass is forced to change with time as to ensure that the ratio between the energy densities of dark matter and dark energy become a constant at late times and one readily realizes that the present-day dark matter abundance is not very sensitive to its value when dark matter particles decouple from the thermal bath. We show that the dependence of the present abundance of cold dark matter on the parameters of the model differs drastically from the familiar results where no connection between dark energy and dark matter is present. In particular, we analyze the case in which the cold dark matter particle is the lightest supersymmetric particle.

Figures (2)

• Figure 1: Time evolution of the relative abundance of different species, expressed as fractions of the critical density. The corresponding parameter configuration is: $\beta=1.88,\,\lambda=0.82,\;\bar{V}=10^2\,{\rm GeV}^4,\; M_S=500\,{\rm GeV},$$M_{\chi}^{\rm ph}=105\,{\rm GeV}$ and $\alpha_S^2=0.0068$
• Figure 2: Regions with $0.1 \leq \Omega_{\chi}h^2 \leq 0.3$ and $M_S > M_{\chi}$ for fixed values of $\Delta \varphi$, see Eq. (\ref{['scaling']}). The grey region represents the parameter space available in the standard scenario $\Delta \varphi=0$. The red+grey region represents the total parameter space available in the VAMP scenario.