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自[https://en.wikipedia.org/wiki/Ludwig_Boltzmann Ludwig Boltzmann]时代以来，熵在宇宙学中的作用仍然是一个有争议的话题。最近的工作使人们对热寂假说以及任何简单的热力学模型在宇宙的普遍适用性产生了怀疑。尽管在扩展的宇宙模型中熵确实增加了，但最大可能的熵却增长得更快，随着时间的推移，使宇宙离热寂的距离越来越远，而不是越来越近。<ref>{{Cite book|last=Layzer|first=David|title=Growth of Order in the Universe|publisher=MIT Press|year=1988}}</ref><ref>{{Cite book|last=Chaisson|first=Eric J.|title=Cosmic Evolution: The Rise of Complexity in Nature|publisher=Harvard University Press|year=2001|isbn=978-0-674-00342-2|url=https://archive.org/details/cosmicevolutionr00chai}}</ref><ref>{{Cite book|editor-last1=Lineweaver|editor-first1=Charles H.|editor-last2=Davies|editor-first2=Paul C. W.|editor-last3=Ruse|editor-first3=Michael|title=Complexity and the Arrow of Time|publisher=Cambridge University Press|year=2013|isbn=978-1-107-02725-1}}</ref> 这导致“熵间隙”，使系统进一步远离假定的热死平衡。<ref>{{Cite book|last=Stenger|first=Victor J.|title=God: The Failed Hypothesis|publisher=Prometheus Books|year=2007|isbn=978-1-59102-481-1}}</ref>其他复杂因素，例如真空的能量密度和宏观量子这种效应很难与热力学模型相吻合，因此热力学对大型系统的任何预测都极为困难。<ref>{{Cite book|author=Benjamin Gal-Or|title=Cosmology, Physics and Philosophy|publisher=Springer Verlag|year=1987|isbn=978-0-387-96526-0}}</ref>

自[https://en.wikipedia.org/wiki/Ludwig_Boltzmann Ludwig Boltzmann]时代以来，熵在宇宙学中的作用仍然是一个有争议的话题。最近的工作使人们对热寂假说以及任何简单的热力学模型在宇宙的普遍适用性产生了怀疑。尽管在扩展的宇宙模型中熵确实增加了，但最大可能的熵却增长得更快，随着时间的推移，使宇宙离热寂的距离越来越远，而不是越来越近。<ref>{{Cite book|last=Layzer|first=David|title=Growth of Order in the Universe|publisher=MIT Press|year=1988}}</ref><ref>{{Cite book|last=Chaisson|first=Eric J.|title=Cosmic Evolution: The Rise of Complexity in Nature|publisher=Harvard University Press|year=2001|isbn=978-0-674-00342-2|url=https://archive.org/details/cosmicevolutionr00chai}}</ref><ref>{{Cite book|editor-last1=Lineweaver|editor-first1=Charles H.|editor-last2=Davies|editor-first2=Paul C. W.|editor-last3=Ruse|editor-first3=Michael|title=Complexity and the Arrow of Time|publisher=Cambridge University Press|year=2013|isbn=978-1-107-02725-1}}</ref> 这导致“熵间隙”，使系统进一步远离假定的热死平衡。<ref>{{Cite book|last=Stenger|first=Victor J.|title=God: The Failed Hypothesis|publisher=Prometheus Books|year=2007|isbn=978-1-59102-481-1}}</ref>其他复杂因素，例如真空的能量密度和宏观量子这种效应很难与热力学模型相吻合，因此热力学对大型系统的任何预测都极为困难。<ref>{{Cite book|author=Benjamin Gal-Or|title=Cosmology, Physics and Philosophy|publisher=Springer Verlag|year=1987|isbn=978-0-387-96526-0}}</ref>

当前的理论表明，熵间隙最初是由宇宙的早期快速[https://en.wikipedia.org/wiki/Inflation_(cosmology) 指数膨胀]所打开的。<ref name="Albrecht">{{cite encyclopedia|last=Albrecht|first=Andreas|author-link=Andreas Albrecht (cosmologist)|editor-last=Barrow|editor-first=John D.|editor-link=John D. Barrow|editor-last2=Davies|editor-first2=Paul C.W.|editor-link2=Paul Davies|editor-last3=Harper |editor-first3=Charles L. Jr.|encyclopedia=Science and Ultimate Reality: From Quantum to Cosmos|title=Cosmic inflation and the arrow of time|url=https://arxiv.org/ftp/astro-ph/papers/0210/0210527.pdf|access-date=28 June 2017|year=2004|publisher=Cambridge University Press|location=Cambridge, UK|arxiv=astro-ph/0210527|postscript=none|bibcode=2002astro.ph.10527A}} (in honor of John

当前的理论表明，熵间隙最初是由宇宙的早期快速[https://en.wikipedia.org/wiki/Inflation_(cosmology) 指数膨胀]所打开的。<ref name="Albrecht">{{cite encyclopedia|last=Albrecht|first=Andreas|editor-last=Barrow|editor-first=John D.|editor-link=John D. Barrow|editor-last2=Davies|editor-first2=Paul C.W.|editor-link2=Paul Davies|editor-last3=Harper |editor-first3=Charles L. Jr.|encyclopedia=Science and Ultimate Reality: From Quantum to Cosmos|title=Cosmic inflation and the arrow of time|url=https://arxiv.org/ftp/astro-ph/papers/0210/0210527.pdf|access-date=28 June 2017|year=2004|publisher=Cambridge University Press|location=Cambridge, UK|arxiv=astro-ph/0210527|postscript=none|bibcode=2002astro.ph.10527A}} (in honor of John

Wheeler’s 90th birthday)</ref>

Wheeler’s 90th birthday)</ref>