Abstract
There is a missing energy problem in cosmology: the total energy density of the Universe, based on a wide range of observations, is much greater than the energy density contributed by all baryons, neutrinos, photons, and dark matter. Deepening this mystery are the recent observations of type la supernovae which suggest that the expansion rate of the Universe is accelerating. One possible resolution is the existence of a cosmological constant which fills this energy gap. However, a logical alternative is “quintessence,” a time-dependent, spatially inhomogeneous, negative pressure energy component which drives the cosmic expansion. This lecture will serve as an introduction to the quintessence cosmological scenario.
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Caldwell, R.R. (2001). An Introduction to Quintessence. In: Cline, D.B. (eds) Sources and Detection of Dark Matter and Dark Energy in the Universe. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-04587-9_7
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DOI: https://doi.org/10.1007/978-3-662-04587-9_7
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