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\documentstyle{article} \thispagestyle{empty} \setlength{\topmargin}{3.mm} \setlength{\evensidemargin}{10mm} \setlength{\oddsidemargin}{7mm} \setlength{\textwidth}{155mm} \setlength{\textheight}{225mm} \setlength{\parindent}{0mm} \setlength{\parskip}{4mm} \begin{document} \ \\ \begin{center} {\LARGE {\bf Models of interacting dark energy}}\\ \ \\ {\bf Winfried Zimdahl}$^{1}$\\ \ \\ $^{1}$ \textit{Departamento de F\'{\i}sica, Universidade Federal do Esp\'{\i}rito Santo\\ 29075-910 Vit\'oria, Esp\'{\i}rito Santo, BRAZIL} \end{center} \ \\ We argue that interactions in the dark sector may have a crucial impact on the cosmological dynamics. In particular, the future cosmic evolution may be very different from that predicted by the $\Lambda$CDM model. An example is a scenario in which the currently observed accelerated expansion is a transient phenomenon \cite{transient,cristofher}. In such a context, the interaction plays a twofold role: it has to cancel the ``bare" cosmological constant and, at the same time, it has to induce a temporary accelerated expansion by itself. In another scenario, an interaction may lead to an attractor behavior for the ratio of the energy densities of dark matter and dark energy, shedding new light on the cosmic coincidence problem \cite{ap}. Although this late-time behavior requires an equation of state of the phantom type, a big-rip singularity is avoided. \begin{thebibliography}{99} \bibitem{transient} J.C. Fabris, B. Fraga, N. Pinto-Neto and W. Zimdahl, JCAP \textbf{1004} (2010) 008. \bibitem{cristofher} C. Zu\~niga Vargas, W.S. Hip\'{o}lito-Ricaldi and W. Zimdahl, JCAP 1204, 032 (2012). arXiv:1112.5337. \bibitem{ap} F. Ar\'{e}valo, A.P. Bacalhau and W. Zimdahl, arXiv:1112.5095. \end{thebibliography} \end{document}

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