Variable cosmological constant as a Planck scale effect
Variable cosmological constant as a Planck scale effect
复制标题
DOI：
10.1016/j.physletb.2003.09.016
复制
发表时间：
2003-03
影响因子：
4.4
通讯作者：
I. Shapiro;J. Solà;C. España-Bonet;P. Ruiz-Lapuente
中科院分区：
文献类型：
--
作者：
I. Shapiro;J. Solà;C. España-Bonet;P. Ruiz-Lapuente
我们构造了一个半经典的Friedmann-Lemaektre-Robertson-步行者（FLRW）宇宙学模型.事实证明，由于最重粒子的剩余量子效应，CC在任意低的能量下变得可变，例如，普朗克尺度物理学这些效应在某种意义上是普遍的，因为它们导致了一个与一大类高能理论相同的低能结构。值得注意的是，关于未知高能动力学的不确定性被累积到单个参数ν中，使得模型具有基本的预测能力。未来的Ia型超新星实验（如SNAP）可以验证这个框架是否正确。对于平坦的FLRW情况和一个中等的值ν = 10−2，我们预测在红移z=1-1.5时，ΩΛ的值会增加10-20%，这是SNAP完全可以达到的。
We construct a semiclassical Friedmann–Lemaı̂tre–Robertson–Walker (FLRW) cosmological model assuming a running cosmological constant (CC). It turns out that the CC becomes variable at arbitrarily low energies due to the remnant quantum effects of the heaviest particles, e.g., the Planck scale physics. These effects are universal in the sense that they lead to a low-energy structure common to a large class of high-energy theories. Remarkably, the uncertainty concerning the unknown high-energy dynamics is accumulated into a single parameter ν , such that the model has an essential predictive power. Future Type Ia supernovae experiments (like SNAP) can verify whether this framework is correct. For the flat FLRW case and a moderate value ν∼10−2, we predict an increase of 10–20% in the value of ΩΛat redshifts z=1–1.5 perfectly reachable by SNAP.