在简单弦论模型中寻找暴胀：天体物理学的观点
Searching for Inflation in Simple String Theory Models: An Astrophysical Perspective
摘要：
试图将弦论与天体物理学观测联系起来的努力受到了一个术语的阻碍，在这个术语中，大量令人生畏的东方褶皱、卡勒势等阻碍了宇宙学家试图从最近的文献中计算出特定弦论解的天体物理学观测值。我们试图帮助弥合这一差距，给出了详细的例子，针对天体物理学家和高能理论家一样，如何计算预测熟悉的宇宙学参数时，开始与10维弦论行动的教学阐述。这是通过研究弦论中的暴胀来完成的，因为暴胀是早期宇宙物理学如何确定宇宙学参数的主导范式。我们分析了三个显式弦模型，从最近的文献中，每个包含一个无限数量的“真空”的解决方案。我们对一些自然的候选暴胀子，即所谓的“模场”进行了数值研究，但没有发现暴胀。我们还发现，在最简单的模型中，在适当的场重新定义之后，大量的这些真空的差异仅在于乘以有效暴胀子势的总常数，这种差异既不影响势的形状，也不影响其支持慢卷暴胀的能力。这说明，即使有无限多的真空，也不能保证有膨胀的真空。这可能是我们所研究的模型的简单性造成的。相反，似乎需要更复杂的弦论模型，这表明明确识别弦景观的膨胀子集将是一个挑战。
英文摘要：
Attempts to connect string theory with astrophysical observation are hampered by a jargon barrier, where an intimidating profusion of orientifolds, Kahler potentials, etc. dissuades cosmologists from attempting to work out the astrophysical observables of specific string theory solutions from the recent literature. We attempt to help bridge this gap by giving a pedagogical exposition with detailed examples, aimed at astrophysicists and high energy theorists alike, of how to compute predictions for familiar cosmological parameters when starting with a 10-dimensional string theory action. This is done by investigating inflation in string theory, since inflation is the dominant paradigm for how early universe physics determines cosmological parameters. We analyze three explicit string models from the recent literature, each containing an infinite number of "vacuum" solutions. Our numerical investigation of some natural candidate inflatons, the so-called "moduli fields", fails to find inflation. We also find in the simplest models that, after suitable field redefinitions, vast numbers of these vacua differ only in an overall constant multiplying the effective inflaton potential, a difference which affects neither the potential's shape nor its ability to support slow-roll inflation. This illustrates that even having an infinite number of vacua does not guarantee having inflating ones. This may be an artifact of the simplicity of the models that we study. Instead, more complicated string theory models appear to be required, suggesting that explicitly identifying the inflating subset of the string landscape will be challenging.
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