Topological Inflation, without the Topology
Topological Inflation, without the Topology
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拓扑膨胀，没有拓扑
DOI：
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发表时间：
1996
期刊：
影响因子：
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通讯作者：
Adrian Martin
中科院分区：
文献类型：
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作者：
N. Lepora;Adrian Martin
我们将Linde和Vilenkin的“拓扑膨胀”推广到不稳定的单极子。这允许量子衰变，而不是像拓扑暴胀所要求的那样永远暴胀。这种情况在某些大统一理论中自然发生，例如超对称翻转SU（5）。我们分析的动力学膨胀的单极子，以确定方程的膨胀，另外恢复的规模上的对称性破缺的酒井等人发现数值上的约束。本文的后半部分致力于膨胀不稳定单极的宇宙学-这是非均匀宇宙学的一个例子。我们描述了这样一个周期是如何形成的，以及它膨胀了多久-发现它是一个随机过程。然后，我们推导出宇宙学参数，如密度和温度，在膨胀结束时是如何分布的，以及宇宙如何随着膨胀衰变而重新加热。这项工作的一般结论是，这种膨胀创造了一个相对平坦，均匀和各向同性的宇宙的局部区域，周围环绕着前GUT物质。
We extend the ‘topological inflation’ of Linde and Vilenkin to unstable monopoles. This allows the monopole to decay; not inflating eternally, as topological inflation demands. Such a situation happens naturally in some Grand Unified Theories — such as supersymmetric flipped-SU(5). We analyse analytically the dynamics of inflating monopoles to determine the equations governing the expansion, additionally recovering the bound on the scale of symmetry breaking found numerically by Sakai et. al. The latter half of this paper is devoted to the Cosmology of inflating unstable monopoles — which is an example of an inhomogeneous cosmology. We describe how such a monopole may be formed and how long it inflates for — finding it to be a random process. We then derive how cosmological parameters, such as density and temperature, are distributed at the end of inflation, and how the Universe reheats as the monopole decays. The general conclusion of this work is that such inflation creates a local region of relatively flat, homogenous and isotropic Universe surrounded by pre-GUT matter.