Dark Matter and Energy in the Universe

Details Dark Matter and Energy in the Universe Dark Matter and Energy in the Universe

1999-01-10

arxiv.org/abs/astro-ph/9901109v1

Phys.Scripta T85 (2000) 210-220

Astronomy and Astrophysics

Astrophysics

30 pages LaTeX with 10 eps figures. To be published in Physica Scripta (Proceedings of the Nobel Symposium, Particle Physics a

Scientific paper

10.1238/Physica.Topical.085a0021

For the first time, we have a plausible and complete accounting of matter and energy in the Universe. Expressed a fraction of the critical density it goes like this: neutrinos, between 0.3% and 15%; stars, between 0.3% and 0.6%; baryons (total), 5% +/- 0.5%; matter (total), 40% +/- 10%; smooth, dark energy, 80% +/- 20%; totaling to the critical density (within the errors). This accounting is consistent with the inflationary prediction of a flat Universe and defines three dark-matter problems: Where are the dark baryons? What is the nonbaryonic dark matter? What is the nature of the dark energy? The leading candidate for the (optically) dark baryons is diffuse hot gas; the leading candidates for the nonbaryonic dark matter are slowly moving elementary particles left over from the earliest moments (cold dark matter), such as axions or neutralinos; the leading candidates for the dark energy involve fundamental physics and include a cosmological constant (vacuum energy), a rolling scalar field (quintessence), and a network of light, frustrated topological defects.

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