Heat death of the universe - wikipedia Heat death of the universe This is the current revision of this page, as edited by Rjwilmsi ( talk contribs ) at 11 : 11, 26 August 2017 ( → ‎ Current status : Journal cites :, added 1 Bibcode using AWB ( 12158 ) ). The present address ( URL ) is a permanent link to this version. Revision as of 11 : 11, 26 August 2017 by Rjwilmsi ( talk contribs ) ( → ‎ Current status : Journal cites :, added 1 Bibcode using AWB ( 12158 ) ) ( diff ) ← Previous revision Latest revision ( diff ) Newer revision → ( diff ) For the album by Off Minor, see The Heat Death of the Universe. Part of a series on Physical cosmology Big Bang Universe Age of the universe Chronology of the universe Early universe Inflation Nucleosynthesis Backgrounds Gravitational wave ( GWB ) Microwave ( CMB ) Neutrino ( CNB ) Expansion Future Hubble 's law Redshift Metric expansion of space FLRW metric Friedmann equations Inhomogeneous cosmology Future of an expanding universe Ultimate fate of the universe Components Structure Components Lambda - CDM model Dark energy Dark fluid Dark matter Structure Shape of the universe Galaxy filament Galaxy formation Large quasar group Large - scale structure Reionization Structure formation Experiments BOOMERanG Cosmic Background Explorer ( COBE ) Illustris project Planck space observatory Sloan Digital Sky Survey ( SDSS ) 2dF Galaxy Redshift Survey ( `` 2dF '' ) Wilkinson Microwave Anisotropy Probe ( WMAP ) Scientists Aaronson Alfvén Alpher Bharadwaj Copernicus de Sitter Dicke Ehlers Einstein Ellis Friedman Galileo Gamow Guth Hawking Hubble Lemaître Mather Newton Penrose Penzias Rubin Schmidt Smoot Suntzeff Sunyaev Tolman Wilson Zel'dovich List of cosmologists Subject history Discovery of cosmic microwave background radiation History of the Big Bang theory Religious interpretations of the Big Bang theory Timeline of cosmological theories Category Cosmology portal Astronomy portal The heat death of the universe is a plausible ultimate fate of the universe in which the universe has diminished to a state of no thermodynamic free energy and therefore can no longer sustain processes that increase entropy. Heat death does not imply any particular absolute temperature ; it only requires that temperature differences or other processes may no longer be exploited to perform work. In the language of physics, this is when the universe reaches thermodynamic equilibrium ( maximum entropy ). If the topology of the universe is open or flat, or if dark energy is a positive cosmological constant ( both of which are supported by current data ), the universe will continue expanding forever and a heat death is expected to occur, with the universe cooling to approach equilibrium at a very low temperature after a very long time period. The hypothesis of heat death stems from the ideas of William Thomson, 1st Baron Kelvin, who in the 1850s took the theory of heat as mechanical energy loss in nature ( as embodied in the first two laws of thermodynamics ) and extrapolated it to larger processes on a universal scale. Contents 1 Origins of the idea 1.1 History 2 Current status 3 Time frame for heat death 4 Controversies 5 See also 6 References Origins of the idea Nature timeline view discuss edit - 13 -- -- - 12 -- -- - 11 -- -- - 10 -- -- - 9 -- -- - 8 -- -- - 7 -- -- - 6 -- -- - 5 -- -- - 4 -- -- - 3 -- -- - 2 -- -- - 1 -- -- 0 -- cosmic expansion Earliest light cosmic speed - up Solar System water Single - celled life photosynthesis Multicellular life Land life Earliest gravity Dark energy Dark matter ← Earliest universe ( − 13.80 ) ← Earliest galaxy ← Earliest quasar ← Omega Centauri forms ← Andromeda Galaxy forms ← Milky Way Galaxy spiral arms form ← Alpha Centauri forms ← Earliest Earth ( − 4.54 ) ← Earliest life ← Earliest oxygen ← Atmospheric oxygen ← Earliest sexual reproduction ← Cambrian explosion ← Earliest humans L i f P r i m o r d i a l Axis scale : billions of years. Also see : Human timeline and Life timeline The idea of heat death stems from the second law of thermodynamics, of which one version states that entropy tends to increase in an isolated system. From this, the hypothesis infers that if the universe lasts for a sufficient time, it will asymptotically approach a state where all energy is evenly distributed. In other words, according to this hypothesis, in nature there is a tendency to the dissipation ( energy transformation ) of mechanical energy ( motion ) into thermal energy ; hence, by extrapolation, there exists the view that the mechanical movement of the universe will run down, as work is converted to heat, in time because of the second law. The conjecture that all bodies in the universe cool off, eventually becoming too cold to support life, seems to have been first put forward by the French astronomer Jean - Sylvain Bailly in 1777 in his writings on the history of astronomy and in the ensuing correspondence with Voltaire. In Bailly 's view, all planets have an internal heat and are now at some particular stage of cooling. Jupiter, for instance, is still too hot for life to arise there for thousands of years, while the Moon is already too cold. The final state, in this view, is described as one of `` equilibrium '' in which all motion ceases. The idea of heat death as a consequence of the laws of thermodynamics, however, was first proposed in loose terms beginning in 1851 by William Thomson, 1st Baron Kelvin, who theorized further on the mechanical energy loss views of Sadi Carnot ( 1824 ), James Joule ( 1843 ), and Rudolf Clausius ( 1850 ). Thomson 's views were then elaborated on more definitively over the next decade by Hermann von Helmholtz and William Rankine. History The idea of heat death of the universe derives from discussion of the application of the first two laws of thermodynamics to universal processes. Specifically, in 1851 William Thomson ( Lord Kelvin ) outlined the view, as based on recent experiments on the dynamical theory of heat, that `` heat is not a substance, but a dynamical form of mechanical effect, we perceive that there must be an equivalence between mechanical work and heat, as between cause and effect. '' Lord Kelvin originated the idea of universal heat death in 1852. In 1852, Thomson published On a Universal Tendency in Nature to the Dissipation of Mechanical Energy in which he outlined the rudiments of the second law of thermodynamics summarized by the view that mechanical motion and the energy used to create that motion will tend to dissipate or run down, naturally. The ideas in this paper, in relation to their application to the age of the sun and the dynamics of the universal operation, attracted the likes of William Rankine and Hermann von Helmholtz. The three of them were said to have exchanged ideas on this subject. In 1862, Thomson published `` On the age of the Sun 's heat '', an article in which he reiterated his fundamental beliefs in the indestructibility of energy ( the first law ) and the universal dissipation of energy ( the second law ), leading to diffusion of heat, cessation of useful motion ( work ), and exhaustion of potential energy through the material universe while clarifying his view of the consequences for the universe as a whole. In a key paragraph, Thomson wrote : The result would inevitably be a state of universal rest and death, if the universe were finite and left to obey existing laws. But it is impossible to conceive a limit to the extent of matter in the universe ; and therefore science points rather to an endless progress, through an endless space, of action involving the transformation of potential energy into palpable motion and hence into heat, than to a single finite mechanism, running down like a clock, and stopping for ever. In the years to follow both Thomson 's 1852 and the 1865 papers, Helmholtz and Rankine both credited Thomson with the idea, but read further into his papers by publishing views stating that Thomson argued that the universe will end in a `` heat death '' ( Helmholtz ) which will be the `` end of all physical phenomena '' ( Rankine ). Current status See also : Entropy § Cosmology, and Entropy ( arrow of time ) § Cosmology Proposals about the final state of the universe depend on the assumptions made about its ultimate fate, and these assumptions have varied considerably over the late 20th century and early 21st century. In a hypothesized `` open '' or `` flat '' universe that continues expanding indefinitely, a heat death is expected to occur. If the cosmological constant is zero, the universe will approach absolute zero temperature over a very long timescale. However, if the cosmological constant is positive, as appears to be the case in recent observations, the temperature will asymptote to a non-zero, positive value and the universe will approach a state of maximum entropy. The `` heat death '' situation could be avoided if there is a method or mechanism to regenerate hydrogen atoms from radiation, dark energy or other sources in order to avoid a gradual running down of the universe due to the conversion of matter into energy and heavier elements in stellar processes. Time frame for heat death Main article : Future of an expanding universe From the Big Bang through the present day, matter and dark matter in the universe are thought to have been concentrated in stars, galaxies, and galaxy clusters, and are presumed to continue to be so well into the future. Therefore, the universe is not in thermodynamic equilibrium and objects can do physical work. The decay time for a supermassive black hole of roughly 1 galaxy - mass ( 10 solar masses ) due to Hawking radiation is on the order of 10 years, so entropy can be produced until at least that time. After that time, the universe enters the so - called Dark Era, and is expected to consist chiefly of a dilute gas of photons and leptons. With only very diffuse matter remaining, activity in the universe will have tailed off dramatically, with extremely low energy levels and extremely long time scales. Speculatively, it is possible that the universe may enter a second inflationary epoch, or, assuming that the current vacuum state is a false vacuum, the vacuum may decay into a lower - energy state. It is also possible that entropy production will cease and the universe will reach heat death. Possibly another universe could be created by random quantum fluctuations or quantum tunneling in roughly 10 10 10 56 ( displaystyle 10 ^ ( 10 ^ ( 10 ^ ( 56 ) ) ) ) years. Over an infinite time, there would be a spontaneous entropy decrease via the Poincaré recurrence theorem, thermal fluctuations, and Fluctuation theorem. Controversies Max Planck wrote that the phrase `` entropy of the universe '' has no meaning because it admits of no accurate definition. More recently, Grandy writes : `` It is rather presumptuous to speak of the entropy of a universe about which we still understand so little, and we wonder how one might define thermodynamic entropy for a universe and its major constituents that have never been in equilibrium in their entire existence. '' According to Tisza : `` If an isolated system is not in equilibrium, we can not associate an entropy with it. '' Buchdahl writes of `` the entirely unjustifiable assumption that the universe can be treated as a closed thermodynamic system ''. According to Gallavotti : ``... there is no universally accepted notion of entropy for systems out of equilibrium, even when in a stationary state. '' Discussing the question of entropy for non-equilibrium states in general, Lieb and Yngvason express their opinion as follows : `` Despite the fact that most physicists believe in such a nonequilibrium entropy, it has so far proved impossible to define it in a clearly satisfactory way. '' In the opinion of Čápek and Sheehan, `` no known formulation ( of entropy ) applies to all possible thermodynamic regimes. '' In Landsberg 's opinion, `` The third misconception is that thermodynamics, and in particular, the concept of entropy, can without further enquiry be applied to the whole universe... These questions have a certain fascination, but the answers are speculations, and lie beyond the scope of this book. '' A recent analysis of entropy states that `` The entropy of a general gravitational field is still not known, '' and that `` gravitational entropy is difficult to quantify. '' The analysis considers several possible assumptions that would be needed for estimates, and suggests that the visible universe has more entropy than previously thought. This is because the analysis concludes that supermassive black holes are the largest contributor. Another writer goes further ; `` It has long been known that gravity is important for keeping the universe out of thermal equilibrium. Gravitationally bound systems have negative specific heat -- that is, the velocities of their components increase when energy is removed... Such a system does not evolve toward a homogeneous equilibrium state. Instead it becomes increasingly structured and heterogeneous as it fragments into subsystems. '' See also Arrow of time Big Bang Big Bounce Big Crunch Big Rip Chronology of the universe Cyclic model Entropy ( arrow of time ) Fluctuation theorem Graphical timeline from Big Bang to Heat Death Heat death paradox The Last Question Terasecond and longer References ^ Jump up to : Plait, Philip Death From the Skies !, Viking Penguin, NY, ISBN 978 - 0 - 670 - 01997 - 7, p. 259 Jump up ^ Brush, Stephen G. ( 1996 ). A History of Modern Planetary Physics : Nebulous Earth. Cambridge University Press. p. 77. ISBN 9780521441711. Jump up ^ Thomson, William. ( 1851 ). `` On the Dynamical Theory of Heat, with numerical results deduced from Mr Joule 's equivalent of a Thermal Unit, and M. Regnault 's Observations on Steam. '' Excerpts. ( § § 1 -- 14 & § § 99 -- 100 ), Transactions of the Royal Society of Edinburgh, March, 1851 ; and Philosophical Magazine IV. 1852. ( from Mathematical and Physical Papers, vol. i, art. XLVIII, pp. 174 ) Jump up ^ Thomson, William ( 1852 ). `` On a Universal Tendency in Nature to the Dissipation of Mechanical Energy '' Proceedings of the Royal Society of Edinburgh for April 19, 1852, also Philosophical Magazine, Oct. 1852. ( This version from Mathematical and Physical Papers, vol. i, art. 59, pp. 511. ) ^ Jump up to : Smith, Crosbie & Wise, Matthew Norton. ( 1989 ). Energy and Empire : A Biographical Study of Lord Kelvin. ( pg. 500 ). Cambridge University Press. Jump up ^ Thomson, William. ( 1862 ). `` On the age of the sun 's heat '', Macmillan 's Mag., 5, 288 -- 93 ; PL, 1, 394 -- 68. Jump up ^ Physics Timeline ( Helmholtz and Heat Death, 1854 ) Jump up ^ Lisa Dyson, Matthew Kleban, Leonard Susskind : `` Disturbing Implications of a Cosmological Constant '' Jump up ^ MacMillan, W.D. ( 1918 ). `` On stellar evolution ''. Astrophys. J. 48 : 35 -- 49. Bibcode : 1918ApJ... 48... 35M. doi : 10.1086 / 142412. Jump up ^ Macmillan, William D. ( 1925 ). `` Some Mathematical Aspects of Cosmology ''. Science. 62 ( 1596 ) : 96 -- 9. Bibcode : 1925Sci... 62... 121M. PMID 17752724. doi : 10.1126 / science. 62.1596. 96. ^ Jump up to : Fred C. Adams and Gregory Laughlin ( 1997 ). `` A dying universe : the long - term fate and evolution of astrophysical objects ''. Reviews of Modern Physics. 69 ( 2 ) : 337 -- 372. Bibcode : 1997RvMP... 69... 337A. arXiv : astro - ph / 9701131. doi : 10.1103 / RevModPhys. 69.337... Jump up ^ Particle emission rates from a black hole : Massless particles from an uncharged, nonrotating hole, Don N. Page, Physical Review D 13 ( 1976 ), pp. 198 -- 206. doi : 10.1103 / PhysRevD. 13.198. See in particular equation ( 27 ). Jump up ^ Carroll, Sean M. and Chen, Jennifer ( 2004 ). Carroll, Sean M. ; Chen, Jennifer ( 2004 ). `` Spontaneous Inflation and Origin of the Arrow of Time ''. arXiv : hep - th / 0410270. Jump up ^ http://arxiv.org/pdf/astro-ph/0302131.pdf?origin=publication_detail Jump up ^ Werlang, T. ; Ribeiro, G.A.P. ; Rigolin, Gustavo ( 2012 ). `` Interplay between quantum phase transitions and the behavior of quantum correlations at finite temperatures.org ''. International Journal of Modern Physics B. 27 ( 1345032 ) : 1345032. Bibcode : 2013IJMPB... 2745032W. arXiv : 1205.1046. doi : 10.1142 / S021797921345032X. Jump up ^ Xiu - San Xing ( 1 November 2007 ). `` Spontaneous entropy decrease and its statistical formula ''. ResearchGate. Jump up ^ `` Sinks in the landscape, Boltzmann brains and the cosmological constant problem - Abstract - Journal of Cosmology and Astroparticle Physics - IOPscience ''. iop.org. Jump up ^ Uffink, J. ( 2003 ). Irreversibility and the Second Law of Thermodynamics, Chapter 7 of Entropy, p. 129 of Greven, A., Keller, G., Warnecke ( editors ) ( 2003 ), Entropy, Princeton University Press, Princeton NJ, ISBN 0 - 691 - 11338 - 6. Uffink writes : `` The importance of Planck 's Vorlesungen über Thermodynamik ( Planck 1897 ) can hardly be ( over ) estimated. The book has gone through 11 editions, from 1897 until 1964, and still remains the most authoritative exposition of classical thermodynamics. '' Jump up ^ Planck, M. ( 1897 / 193 ). Treatise on Thermodynamics, translated by A. Ogg, p. 101. Jump up ^ Grandy, W.T. ( Jr ) ( 2008 ). Entropy and the Time Evolution of Macroscopic Systems, Oxford University Press, Oxford UK, ISBN 978 - 0 - 19 - 954617 - 6, p. 151. Jump up ^ Tisza, L. ( 1966 ). Generalized Thermodynamics, M.I.T Press, Cambridge MA, p. 41. Jump up ^ Buchdahl, H.A. ( 1966 ). The Concepts of Classical Thermodynamics, Cambridge University Press, Cambridge UK, p. 97. Jump up ^ Gallavotti, G. ( 1999 ). Short Treatise of Statistical Mechanics, Springer, Berlin, ISBN 9783540648833, p. 290. Jump up ^ Lieb, E.H., Yngvason, J. ( 2003 ). The entropy of classical thermodynamics, Chapter 8 of Greven, A., Keller, G., Warnecke ( editors ) ( 2003 ). Entropy, Princeton University Press, Princeton NJ, ISBN 0 - 691 - 11338 - 6, page 190. Jump up ^ Čápek, V., Sheehan, D.P. ( 2005 ). Challenges to the Second Law of Thermodynamics : Theory and Experiment, Springer, Dordrecht, ISBN 1 - 4020 - 3015 - 0, p. 26. Jump up ^ Landsberg, P.T. ( 1961 ). Thermodynamics, with Quantum Statistical Illustrations, Wiley, New York, p. 391. Jump up ^ Egan, Chas A. ; Lineweaver, Charles H. ( 2009 ). `` A Larger Estimate of the Entropy of the Universe ''. The Astrophysical Journal. 710 ( 2 ) : 1825 -- 1834. Bibcode : 2010ApJ... 710.1825 E. arXiv : 0909.3983. doi : 10.1088 / 0004 - 637X / 710 / 2 / 1825. Jump up ^ Smolin, L. ( 2014 ). `` Time, laws, and future of cosmology ''. Physics Today. 67 ( 3 ) : 38 -- 43 ( 42 ). Bibcode : 2014PhT... 67c... 38S. doi : 10.1063 / pt. 3.2310. Timeline of the Big Bang Chronology of the universe Big Bang Planck epoch Grand unification epoch Electroweak epoch ( Inflationary epoch, Reheating, Baryogenesis ) Quark epoch Hadron epoch Lepton epoch Photon epoch ( Big Bang nucleosynthesis, Matter domination, Recombination ) Dark ages Habitable epoch Reionization Fate of the universe Big Crunch Big Rip Heat death of the universe Graphical timeline of the Big Bang Cosmology portal Astronomy portal Solar System portal Space portal Retrieved from `` https://en.wikipedia.org/w/index.php?title=Heat_death_of_the_universe&oldid=797333528 '' Categories : Physical cosmology Eschatology Thermodynamic entropy Doomsday scenarios 1851 in science Hidden categories : Wikipedia semi-protected pages All articles with unsourced statements Articles with unsourced statements from November 2015 Articles with unsourced statements from August 2016 Talk Article Talk View source More Contents About Wikipedia العربية Български Čeština Dansk Deutsch Español فارسی Français 한국어 Italiano עברית Lietuvių Nederlands 日本 語 Norsk Polski Português Русский Slovenčina Suomi Svenska Українська Tiếng Việt 中文 Edit links This page was last edited on 26 August 2017, at 11 : 11. 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Question: the heat death of the universe is a theoretical time in the future when the universe is supposed to
Answer: diminished to a state of no thermodynamic free energy