The following sections of this BookRags Literature Study Guide is offprint from Gale's For Students Series: Presenting Analysis, Context, and Criticism on Commonly Studied Works: Introduction, Author Biography, Plot Summary, Characters, Themes, Style, Historical Context, Critical Overview, Criticism and Critical Essays, Media Adaptations, Topics for Further Study, Compare & Contrast, What Do I Read Next?, For Further Study, and Sources.
(c)1998-2002; (c)2002 by Gale. Gale is an imprint of The Gale Group, Inc., a division of Thomson Learning, Inc. Gale and Design and Thomson Learning are trademarks used herein under license.
The following sections, if they exist, are offprint from Beacham's Encyclopedia of Popular Fiction: "Social Concerns", "Thematic Overview", "Techniques", "Literary Precedents", "Key Questions", "Related Titles", "Adaptations", "Related Web Sites". (c)1994-2005, by Walton Beacham.
The following sections, if they exist, are offprint from Beacham's Guide to Literature for Young Adults: "About the Author", "Overview", "Setting", "Literary Qualities", "Social Sensitivity", "Topics for Discussion", "Ideas for Reports and Papers". (c)1994-2005, by Walton Beacham.
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Cosmological heat death is the name given to the fate of the universe if it continues to expand forever. In standard cosmological models, the universe is finite, so it has a finite amount of energy. Because the universe is expanding, the energy is being spread throughout a larger and larger volume; less energy in a given volume means that the temperature in that volume is decreasing. Eventually, the energy density becomes so low that the temperature approaches absolute zero. At this point, heat death sets in and, for all practical purposes, all activity ceases from that time onward.
Soon after the discovery of general relativity by Albert Einstein in 1915, the theory was applied to the entire universe by Friedmann, Robertson, and Walker (FRW). The solution of Einstein's equations in this case predicted that the universe was expanding, prompting Einstein to introduce his flawed cosmological constant to counteract the expansion. Edwin Hubble's 1929 discovery that the universe was indeed expanding embarrassed Einstein, but opened up a new era in cosmological predictions.
The most important parameter in the FRW model is the density of the universe today. A critical density determines whether the universe will eventually contract back to a point (the big crunch) or whether it will continue expanding forever. If the density is greater than the critical density, the universe will at some point begin to contract. If the density is less than the critical density, then the universe will expand forever at an accelerating rate. If the density is equal to the critical density, then the expansion will continue forever but will approach zero after a long time.
When the density is less than or equal to the critical density, the expansion never stops, leading to cosmological heat death. Based on current observations, this heat death should occur when the universe is about 1098 years old; at this time, galactic black holes will evaporate, leaving no observable structure in the universe. The universe is about 1010 years old now, so it is highly unlikely that humans will exist to observe the occurrence of the heat death.