更改

== 热寂的时间范围 ==

== 热寂的时间范围 ==

从大爆炸到今天，我们认为宇宙中的物质和暗物质集中在恒星、星系和星系团中，并且推测未来依然如此。因此，宇宙并未处于热力学平衡状态，物体可以做功<ref name=":0">Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: the long-term fate and evolution of astrophysical objects". ''Reviews of Modern Physics''. '''69''' (2): 337–72. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID 12173790</ref>。由于霍金辐射，一个大约1个星系质量（10¹¹个太阳质量）的超大质量黑洞的衰减时间是10¹⁰⁰年左右<ref>See in particular equation (27) in Page, Don N. (15 January 1976). "Particle emission rates from a black hole: Massless particles from an uncharged, nonrotating hole". ''Physical Review D''. '''13''' (2): 198–206. Bibcode:1976PhRvD..13..198P. doi:10.1103/PhysRevD.13.198.</ref>，所以熵至少可以产生到那个时候。据预测，宇宙中的一些大型黑洞在星系超级星系团的坍缩过程中会继续增长，最大可能达到10¹⁴M☉。即使是这些黑洞，也会在长达10¹⁰⁶年的时间范围内消失<ref>Frautschi, Steven (13 August 1982). "Entropy in an Expanding Universe" (PDF). ''Science''. '''217''' (4560): 593–9. Bibcode:1982Sci...217..593F. doi:10.1126/science.217.4560.593. JSTOR 1688892. <nowiki>PMID 17817517</nowiki>. S2CID 27717447. <q>Since we have assumed a maximum scale of gravitational binding—for instance, superclusters of galaxies—black hole formation eventually comes to an end in our model, with masses of up to 10¹⁴<var>M</var>_☉ ... the timescale for black holes to radiate away all their energy ranges ... to 10¹⁰⁶ years for black holes of up to 10¹⁴<var>M</var>_☉</q></ref>。在那之后，宇宙就进入了所谓的黑暗时代，预计将主要由光子和轻子的稀薄气体组成<ref name=":0" />。由于只剩下非常分散的物质，宇宙的活动将急剧减少，能量水平极低，时间尺度极长。从推测上看，宇宙有可能进入第二个膨胀时代，或者假设目前的真空状态是假真空，那么真空可能会衰变为低能量状态<ref name=":0" />。也有可能，熵的产生将停止，宇宙将达到热寂<ref name=":0" /><nowiki>。另一个宇宙可能是由随机量子波动或量子隧道在大约{\displaystyle 10^{10^{10^{56}}}}10^{10^{10^{56}}}年内产生的</nowiki><ref>Carroll, Sean M.; Chen, Jennifer (October 2004). "Spontaneous Inflation and Origin of the Arrow of Time". Bibcode:2004hep.th...10270C</ref>。有人认为，在漫长的时间里，自发的熵减少最终会庞加莱递归定理<ref>Poincaré, Henri (1890). "Sur le problème des trois corps et les équations de la dynamique". ''Acta Mathematica''. '''13''': A3–A270.</ref>、热波动<ref>Tegmark, Max (2003). "Parallel Universes". ''Scientific American''. '''288''' (2003): 40–51. arXiv:astro-ph/0302131. Bibcode:2003SciAm.288e..40T. doi:10.1038/scientificamerican0503-40. <nowiki>PMID 12701329</nowiki>.</ref><ref>Tegmark, Max (May 2003). "Parallel Universes". ''Scientific American''. '''288''' (5): 40–51. arXiv:astro-ph/0302131. Bibcode:2003SciAm.288e..40T. doi:10.1038/scientificamerican0503-40<nowiki/>PMID 12701329</ref><ref>Werlang, T.; Ribeiro, G. A. P.; Rigolin, Gustavo (2013). "Interplay between quantum phase transitions and the behavior of quantum correlations at finite temperatures". ''International Journal of Modern Physics B''. '''27''' (1n03): 1345032. arXiv:1205.1046. Bibcode:2013IJMPB..2745032W. doi:10.1142/S021797921345032X. S2CID 119264198.</ref>、和波动定理<ref>Xiu-San Xing (1 November 2007). "Spontaneous entropy decrease and its statistical formula". arXiv:0710.4624 [cond-mat.stat-mech].</ref><ref>Linde, Andrei (2007). "Sinks in the landscape, Boltzmann brains and the cosmological constant problem". ''Journal of Cosmology and Astroparticle Physics''. '''2007''' (1): 022. arXiv:hep-th/0611043. Bibcode:2007JCAP...01..022L. CiteSeerX 10.1.1.266.8334. doi:10.1088/1475-7516/2007/01/022. S2CID 16984680.</ref>的作用下发生。然而，这种情况被描述为 "高度推测，很可能是错误的，[而且]完全无法测试。<ref>Pimbblet, Kevin (3 September 2015). "The fate of the universe: heat death, Big Rip or cosmic consciousness?". ''The Conversation''.</ref>"肖恩-M-卡罗尔最初是这种想法的倡导者，但现在不再支持它了<ref>Carroll, Sean (27 January 2014). ''Sean Carroll, "Fluctuations in de Sitter Space" FQXi conference 2014 in Vieques''. FQXi.</ref><ref>Boddy, Kimberly K.; Carroll, Sean M.; Pollack, Jason (2014). "De Sitter Space Without Dynamical Quantum Fluctuations". arXiv:1405.0298 [hep-th].</ref>。

从大爆炸到今天，我们认为宇宙中的物质和暗物质集中在恒星、星系和星系团中，并且推测未来依然如此。因此，宇宙并未处于热力学平衡状态，物体可以做功<ref name=":0">Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: the long-term fate and evolution of astrophysical objects". ''Reviews of Modern Physics''. '''69''' (2): 337–72. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID 12173790</ref>。由于霍金辐射，一个大约1个星系质量（10¹¹个太阳质量）的超大质量黑洞的衰减时间是10¹⁰⁰年左右<ref>See in particular equation (27) in Page, Don N. (15 January 1976). "Particle emission rates from a black hole: Massless particles from an uncharged, nonrotating hole". ''Physical Review D''. '''13''' (2): 198–206. Bibcode:1976PhRvD..13..198P. doi:10.1103/PhysRevD.13.198.</ref>，所以熵至少可以产生到那个时候。据预测，宇宙中的一些大型黑洞在星系超级星系团的坍缩过程中会继续增长，最大可能达到10¹⁴M☉。即使是这些黑洞，也会在长达10¹⁰⁶年的时间范围内消失<ref>Frautschi, Steven (13 August 1982). "Entropy in an Expanding Universe" (PDF). ''Science''. '''217''' (4560): 593–9. Bibcode:1982Sci...217..593F. doi:10.1126/science.217.4560.593. JSTOR 1688892. <nowiki>PMID 17817517</nowiki>. S2CID 27717447. <q>Since we have assumed a maximum scale of gravitational binding—for instance, superclusters of galaxies—black hole formation eventually comes to an end in our model, with masses of up to 10¹⁴<var>M</var>_☉ ... the timescale for black holes to radiate away all their energy ranges ... to 10¹⁰⁶ years for black holes of up to 10¹⁴<var>M</var>_☉</q></ref>。在那之后，宇宙就进入了所谓的黑暗时代，预计将主要由光子和轻子的稀薄气体组成<ref name=":0" />。由于只剩下非常分散的物质，宇宙的活动将急剧减少，能量水平极低，时间尺度极长。从推测上看，宇宙有可能进入第二个膨胀时代，或者假设目前的真空状态是假真空，那么真空可能会衰变为低能量状态<ref name=":0" />。也有可能，熵的产生将停止，宇宙将达到热寂<ref name=":0" /><nowiki>。另一个宇宙可能是由随机量子波动或量子隧道在大约[math]{\displaystyle 10^{10^{10^{56}}}}[/math]年内产生的</nowiki><ref>Carroll, Sean M.; Chen, Jennifer (October 2004). "Spontaneous Inflation and Origin of the Arrow of Time". Bibcode:2004hep.th...10270C</ref>。有人认为，在漫长的时间里，自发的熵减少最终会庞加莱递归定理<ref>Poincaré, Henri (1890). "Sur le problème des trois corps et les équations de la dynamique". ''Acta Mathematica''. '''13''': A3–A270.</ref>、热波动<ref>Tegmark, Max (2003). "Parallel Universes". ''Scientific American''. '''288''' (2003): 40–51. arXiv:astro-ph/0302131. Bibcode:2003SciAm.288e..40T. doi:10.1038/scientificamerican0503-40. <nowiki>PMID 12701329</nowiki>.</ref><ref>Tegmark, Max (May 2003). "Parallel Universes". ''Scientific American''. '''288''' (5): 40–51. arXiv:astro-ph/0302131. Bibcode:2003SciAm.288e..40T. doi:10.1038/scientificamerican0503-40<nowiki/>PMID 12701329</ref><ref>Werlang, T.; Ribeiro, G. A. P.; Rigolin, Gustavo (2013). "Interplay between quantum phase transitions and the behavior of quantum correlations at finite temperatures". ''International Journal of Modern Physics B''. '''27''' (1n03): 1345032. arXiv:1205.1046. Bibcode:2013IJMPB..2745032W. doi:10.1142/S021797921345032X. S2CID 119264198.</ref>、和波动定理<ref>Xiu-San Xing (1 November 2007). "Spontaneous entropy decrease and its statistical formula". arXiv:0710.4624 [cond-mat.stat-mech].</ref><ref>Linde, Andrei (2007). "Sinks in the landscape, Boltzmann brains and the cosmological constant problem". ''Journal of Cosmology and Astroparticle Physics''. '''2007''' (1): 022. arXiv:hep-th/0611043. Bibcode:2007JCAP...01..022L. CiteSeerX 10.1.1.266.8334. doi:10.1088/1475-7516/2007/01/022. S2CID 16984680.</ref>的作用下发生。然而，这种情况被描述为 "高度推测，很可能是错误的，[而且]完全无法测试。<ref>Pimbblet, Kevin (3 September 2015). "The fate of the universe: heat death, Big Rip or cosmic consciousness?". ''The Conversation''.</ref>"肖恩-M-卡罗尔最初是这种想法的倡导者，但现在不再支持它了<ref>Carroll, Sean (27 January 2014). ''Sean Carroll, "Fluctuations in de Sitter Space" FQXi conference 2014 in Vieques''. FQXi.</ref><ref>Boddy, Kimberly K.; Carroll, Sean M.; Pollack, Jason (2014). "De Sitter Space Without Dynamical Quantum Fluctuations". arXiv:1405.0298 [hep-th].</ref>。

== 反对观点 ==

== 反对观点 ==