An introduction to quintessence

Please use this identifier to cite or link to this item: http://dspace.mediu.edu.my:8181/xmlui/handle/123456789/2909

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DC Field	Value	Language
dc.creator	Caldwell R. R.	-
dc.date	2000	-
dc.date.accessioned	2013-05-29T23:54:05Z	-
dc.date.available	2013-05-29T23:54:05Z	-
dc.date.issued	2013-05-30	-
dc.identifier	http://www.scielo.br/scielo.php?script=sci_arttext&pid=S0103-97332000000200002	-
dc.identifier	http://www.doaj.org/doaj?func=openurl&genre=article&issn=01039733&date=2000&volume=30&issue=2&spage=215	-
dc.identifier.uri	http://koha.mediu.edu.my:8181/jspui/handle/123456789/2909	-
dc.description	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 1a 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.	-
dc.publisher	Sociedade Brasileira de Física	-
dc.source	Brazilian Journal of Physics	-
dc.title	An introduction to quintessence	-
Appears in Collections:	Physics and Astronomy

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