Dark energy and dark matter

By D. Comelli, M. Pietroni, A. Riotto. 2003

212 citations recorded by the source corpus.

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 Letter 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/52a23b5bccb305c37bc19f60005d4f9688815a80

How researchers see this paper

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In Astronomy and Astrophysics

1. G. Farrar
2. A. Nelson
3. N. Weiner
4. P. Peebles
5. M. White
6. R. Scoccimarro
7. L. Widrow
8. Pierre-Henri Chavanis

In Nuclear and High Energy Physics

1. G. Farrar
2. A. Nelson
3. N. Weiner
4. P. Peebles
5. Jonathan L. Feng
6. I. Low
7. Tiberiu Harko
8. M. Setare

In Statistical and Nonlinear Physics

1. A. Nelson
2. N. Weiner
3. Jonathan L. Feng
4. D. Mattingly

Citations in the corpus

• Dark energy from mass varying neutrinos (2003, background): “Variable mass particles were proposed to solve the age of the universe problem in ref. [38], and more recently as a solution to the problem of the coincidence of dark matter and dark energy densities [41]. Phenomenological problems with this have been studied in [42–44]. In the context of neutrinos,”
• Dark energy from backreaction (2003, unknown): “-k”
• Interacting Dark Matter and Dark Energy (2003, background): “In the solution for fi ¼ 1 and ¼ 2, plotted as the long-dashed curves in Figures 1 and 3, the growth of the 7 Anderson & Carroll (1997) and Comelli et al. (2003) consider the case that the scalar field sits at the minimum of the effective potential.”