Evolution of vacuum fluctuations generated during and before inflation
Evolution of vacuum fluctuations generated during and before inflation
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膨胀期间和之前产生的真空波动的演变
DOI：
10.1103/physrevd.89.103536
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
S. Iso and Y. Sekino
中科院分区：
文献类型：
--
作者：
H. Aoki;S. Iso and Y. Sekino
我们计算的期望值的能量动量张量的时间演化的最小耦合无质量标量场在宇宙时空中，与暗能量的应用。我们首先研究了从暴胀到现在的演化，固定Bunch-Davies初始条件。量子场的能量密度在物质主导周期内演化，其中和是暴胀期间和每个时刻的哈勃参数。其状态方程在辐射主导（RD）期由负值到，在MD期由负值到。然后，我们考虑可能的影响普朗克宇宙，这可能已经存在的通货膨胀之前，通过假设有另一个通货膨胀与哈勃参数。在这种情况下，波长大于当前视界半径的模式主要被放大，并且量子场的能量密度随着时间增长，如在MD周期中，其中和是在每个时间和当前的标度因子。因此，如果是普朗克尺度的量级，就可以和现在的临界密度相比较。在自由场近似下，在普通暴胀之前产生的长波涨落的贡献是很大的。我们提到了一种可能性，即相互作用进一步放大了能量密度并改变了状态方程。
We calculate the time evolution of the expectation value of the energy-momentum tensor for a minimally coupled massless scalar field in cosmological spacetimes, with an application to dark energy in mind. We first study the evolution from inflation until the present, fixing the Bunch-Davies initial condition. The energy density of a quantum field evolves asin the matter-dominated (MD) period, whereandare the Hubble parameters during inflation and at each moment. Its equation of state,, changes from a negative value toin the radiation-dominated (RD) period, and fromtoin the MD period. We then consider possible effects of a Planckian universe, which may have existed before inflation, by assuming there was another inflation with the Hubble parameter. In this case, modes with wavelengths longer than the current horizon radius are mainly amplified, and the energy density of a quantum field grows with time asin the MD period, whereandare the scale factors at each time and at present. Hence, ifis of the order of the Planck scale,becomes comparable to the critical densityat the present time. The contribution tofrom the long wavelength fluctuations generated before the ordinary inflation hasin the free field approximation. We mention a possibility that interactions further amplify the energy density and change the equation of state.
慢滚膨胀过程中量子涨落的随机增长
DOI：
10.1103/physrevd.82.064020
发表时间：
2010
期刊：
arXiv: High Energy Physics - Theory
影响因子：
--
作者：
F. Finelli;G. Marozzi;A. Starobinsky;G. Vacca;G. Venturi
通讯作者：
G. Venturi
三阶段宇宙中量子场、粒子含量和经典性的演化
影响因子：
5
作者：
Suprit Singh;Sujoy K. Modak;T. Padmanabhan
通讯作者：
T. Padmanabhan