Inflation and de Sitter thermodynamics
Inflation and de Sitter thermodynamics
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DOI：
10.1088/1475-7516/2003/05/009
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发表时间：
2002-12
影响因子：
6.4
通讯作者：
A. Frolov;L. Kofman
中科院分区：
文献类型：
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作者：
A. Frolov;L. Kofman
我们考虑暴胀宇宙的准德西特几何。我们计算了缓慢滚动的背景标量场通过准de Sitter视视界的能流，并将其设为熵的变化（面积的1/4）乘以温度，dE = TdS。值得注意的是，这个热力学定律再现了滚动标量场的弗里德曼方程。通过准德西特几何视界的缓慢滚动场的通量类似于滚动标量场到黑洞上的吸积，我们也对此进行了分析。接下来，我们加入暴胀子涨落，产生标量度量扰动。度规扰动导致面积熵的变化。同样，方程dE = TdS与波动再现线性化的爱因斯坦方程。在这幅图中，只要爱因斯坦方程成立，全息术就不会在暴胀期间限制量子场论。由于累积的度规扰动，暴胀期间的视界面积随色散随时间增加而随机摆动。我们讨论这与通货膨胀的随机描述。我们还解决了问题的不稳定性暴胀子波动的“热锡罐”图片德西特地平线。
We consider the quasi-de Sitter geometry of the inflationary universe. We calculate the energy flux of the slowly rolling background scalar field through the quasi-de Sitter apparent horizon and set it equal to the change of the entropy (1/4 of the area) multiplied by the temperature, dE = TdS. Remarkably, this thermodynamic law reproduces the Friedmann equation for the rolling scalar field. The flux of the slowly rolling field through the horizon of the quasi-de Sitter geometry is similar to the accretion of a rolling scalar field onto a black hole, which we also analyse. Next we add inflaton fluctuations which generate scalar metric perturbations. Metric perturbations result in a variation of the area entropy. Again, the equation dE = TdS with fluctuations reproduces the linearized Einstein equations. In this picture as long as the Einstein equations hold, holography does not put limits on the quantum field theory during inflation. Due to the accumulating metric perturbations, the horizon area during inflation randomly wiggles with dispersion increasing with time. We discuss this in connection with the stochastic description of inflation. We also address the issue of the instability of inflaton fluctuations in the `hot tin can' picture of the de Sitter horizon.