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{{Original research|date=September 2020}}

{{Original research|date=September 2020}}

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{{Physical cosmology|expansion}}

{{Physical cosmology|expansion}}

The '''heat death of the universe''', also known as the '''Big Chill''' or '''Big Freeze''',<ref>[http://map.gsfc.nasa.gov/universe/uni_fate.html WMAP – Fate of the Universe], ''WMAP's Universe'', [[NASA]]. Accessed online July 17, 2008.</ref> is a [[conjecture]] on the [[ultimate fate of the universe]], which suggests the [[universe]] would evolve to a state of no [[thermodynamic free energy]] and would therefore be unable to sustain processes that increase [[entropy]]. Heat death does not imply any particular [[Thermodynamic temperature#Internal energy at absolute zero|absolute temperature]]; it only requires that temperature differences or other processes may no longer be exploited to perform [[work (thermodynamics)|work]]. In the language of [[physics]], this is when the universe reaches [[thermodynamic equilibrium]] (maximum entropy).

'''宇宙的热寂'''，也被称为大寒或大冻结<ref>[http://map.gsfc.nasa.gov/universe/uni_fate.html WMAP – Fate of the Universe], ''WMAP's Universe'', [[NASA]]. Accessed online July 17, 2008.</ref>，是对宇宙最终命运的猜测，这表明宇宙将进化到没有热力学自由能的状态，因此将无法维持熵增的过程。热寂并不意味着任何特定的绝对温度; 它只要求温差或其他过程可能不再被利用来进行做工。用物理学的语言来说，此时宇宙达到热力学平衡（最大熵）。

 

 

宇宙的热死亡，也被称为大寒或大冻结，是对宇宙最终命运的猜测，这表明宇宙将进化到没有热力学自由能的状态，因此将无法维持增加熵的过程。热死并不意味着任何特定的绝对温度; 它只要求温差或其他过程可能不再利用进行工作。用物理学的语言来说，这是宇宙达到最大熵的热力学平衡。

 

 

 

If the topology of the universe is open or flat, or if dark energy is a positive cosmological constant (both of which are consistent with 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.

If the topology of the universe is open or flat, or if dark energy is a positive cosmological constant (both of which are consistent with 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.

虽然机械能是坚不可摧的，但是它的耗散有一种普遍的趋势，这种趋势使整个系统产生热量的逐渐增加和扩散、运动停止和物质宇宙的势能耗尽。

虽然机械能是坚不可摧的，但是它的耗散有一种普遍的趋势，这种趋势使整个系统产生热量的逐渐增加和扩散、运动停止和物质宇宙的势能耗尽。

}}</ref> with the universe cooling to approach equilibrium at a very low temperature after a very long time period.

}}</ref>。也就是说，宇宙在很长一段时间后会冷却到很低的温度保持平衡。

 

—Thomson, William. [http://zapatopi.net/kelvin/papers/on_the_age_of_the_suns_heat.html On the Age of the Sun’s Heat] Macmillan's Magazine, 5&nbsp;March 1862, pp. 388–93

—Thomson, William. [http://zapatopi.net/kelvin/papers/on_the_age_of_the_suns_heat.html On the Age of the Sun’s Heat] Macmillan's Magazine, 5&nbsp;March 1862, pp. 388–93

ー汤姆森，威廉。《 http://zapatopi.net/kelvin/papers/on_the_age_of_the_suns_heat.html 志，1862年3月5日，页。388–93

ー汤姆森，威廉。论太阳热能的年龄 http://zapatopi.net/kelvin/papers/on_the_age_of_the_suns_heat.html 麦克米伦杂志，1862年3月5日，388–93页

 

The hypothesis of heat death stems from the ideas of [[William Thomson, 1st Baron Kelvin|Lord 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 [[Extrapolation|extrapolated]] it to larger processes on a universal scale.

The hypothesis of heat death stems from the ideas of [[William Thomson, 1st Baron Kelvin|Lord 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 [[Extrapolation|extrapolated]] it to larger processes on a universal scale.

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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 heating|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.<ref>

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 heating|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.<ref>

In the years to follow both Thomson's 1852 and the 1862 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).

In the years to follow both Thomson's 1852 and the 1862 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).

最近在一个相对简单的封闭系统中实验发现了稳定的非平衡稳态，这也支持了这一观点。可以预期的是，一个分裂成子系统的孤立系统不一定会达到热力学平衡并保持非平衡的稳定状态。熵将从一个子系统传递到另一个子系统，但是它的产出将为零，这与热力学第二定律并不矛盾。

最近在一个相对简单的封闭系统中实验发现了稳定的非平衡稳态，这也支持了这一观点。可以预期的是，一个分裂成子系统的孤立系统不一定会达到热力学平衡并保持非平衡的稳定状态。熵将从一个子系统传递到另一个子系统，但是它的产出将为零，这与热力学第二定律并不矛盾。

[[Image:Lord Kelvin photograph.jpg|175px|right|thumb|[[William Thomson, 1st Baron Kelvin|Lord Kelvin]] originated the idea of universal heat death in 1852.]]

[[Image:Lord Kelvin photograph.jpg|175px|right|thumb|[[William Thomson, 1st Baron Kelvin|Lord Kelvin]] originated the idea of universal heat death in 1852.|链接=Special:FilePath/Lord_Kelvin_photograph.jpg]]

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 naturally tend to dissipate or run down.<ref>Thomson, Sir William (1852). [https://zapatopi.net/kelvin/papers/on_a_universal_tendency.html "On a Universal Tendency in Nature to the Dissipation of Mechanical Energy"] ''[[Proceedings of the Royal Society of Edinburgh]]'' for 19 April 1852, also ''[[Philosophical Magazine]]'', Oct. 1852. [This version from ''Mathematical and Physical Papers'', vol. i, art. 59, pp. 511.]</ref> 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.<ref name="Energy and Empire">

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 naturally tend to dissipate or run down.<ref>Thomson, Sir William (1852). [https://zapatopi.net/kelvin/papers/on_a_universal_tendency.html "On a Universal Tendency in Nature to the Dissipation of Mechanical Energy"] ''[[Proceedings of the Royal Society of Edinburgh]]'' for 19 April 1852, also ''[[Philosophical Magazine]]'', Oct. 1852. [This version from ''Mathematical and Physical Papers'', vol. i, art. 59, pp. 511.]</ref> 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.<ref name="Energy and Empire">

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