String Cosmology: New Tools to connect String Theory with Cosmological Observations

弦宇宙学：连接弦理论与宇宙学观测的新工具

• 批准号: ST/H005498/1
• 负责人: Gianmassimo Tasinato
• 金额: $ 53.03万
• 依托单位: University of Portsmouth
• 依托单位国家: 英国
• 项目类别: Fellowship
• 财政年份: 2010
• 资助国家: 英国
• 起止时间: 2010 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FH005498%2F1
• 关键词: String; Cosmology; New; Tools; connect

Cosmology studies the origin of the Universe, and the main features of its evolution until today. The Universe expansion is mainly controlled by gravity, the force described by Einstein's General Relativity. This theory is extremely successful for describing gravitational phenomena that occur at large distances. However, when attempting to describe phenomena occurring at small scales, General Relativity apparently fails. Indeed, the best theories we have to describe short distance physics are based on Quantum Mechanics. But its principles lead to inconsistent results, when applied to gravitational phenomena following the rules of General Relativity. This problem is relevant for Cosmology, when trying to investigate epochs in which the Universe was very young, and then very small, in which quantum mechanical effects are important. For example, in the early epochs of our Universe, it is believed that cosmological expansion has experienced a phase of extremely fast acceleration, called Inflation. During this epoch, quantum effects are decisive to produce small inhomogeneities in the structure of the space-time, that seed large scale structures in the subsequent evolution of the Universe. The aim of consistently conjugate General Relativity with Quantum Mechanics is the main goal that motivated the development of String Theory. This theory introduces very unusual concepts: its consistency requires that our Universe has six dimensions more than the observed ones, that are wrapped on a small space, and unobservable by everyday experience. Also, it predicts the existence of membrane objects, fluctuating in a higher dimensional background, where the particle constituting our Universe can be localized. In order to check these beautiful ideas, however, we need to probe phenomena happening at extremely small scales. I find all these ideas extremely exciting, so I decided to study the relation between string theory and cosmology, with the main aim to find new ways to test string theory by cosmological observations. As explained before, phenomena occurring at early epochs, when the Universe was extremely small, are affected by short distance physics, and then possibly by String Theory. Inflation is the most important example: it is a process that leaves clear imprints in the pattern of the observed CMB radiation, and provides initial conditions affecting the subsequent evolution of the Universe. For these reasons part of my research is devoted to study models of inflation in String Theory. They can have peculiar properties, since they use many of the ingredients that the theory offers. The study of string models of inflation, then, offers unique opportunities to reveal effects that are characteristic of String Theory, and allows to test its ideas by means of cosmological observations. More specifically, the main objectives of my research activity can by summarized in the following. First, I plan to develop the theoretical tools allowing to compare observational results with string motivated cosmological models. This is a broad subject that requires the elaboration of existing techniques aimed to analyze the evolution of cosmological fluctuations, in order to apply them to string motivated cosmological models. Then, I will try to individuate the most promising cosmological models, based on string theory, that offer the best opportunities for being testable with future cosmological observations. Once this has been done, I will try to elaborate those models, in order to render them fully satisfactory from a theoretical point of view, and study in detail their predictions for cosmological quantities that will be tested by observations.

宇宙学研究宇宙的起源，以及直到今天宇宙演化的主要特征。宇宙的膨胀主要是由引力控制的，引力是爱因斯坦广义相对论所描述的力。这个理论对于描述发生在很远距离的引力现象是非常成功的。然而，当试图描述发生在小尺度上的现象时，广义相对论显然失败了。事实上，我们描述短距离物理的最好理论是基于量子力学的。但是，当它的原理应用于遵循广义相对论规则的引力现象时，会导致不一致的结果。这个问题与宇宙学有关，当试图研究宇宙非常年轻的时代时，然后非常小，量子力学效应很重要。例如，在我们宇宙的早期，人们认为宇宙膨胀经历了一个极快的加速阶段，称为暴胀。在这一时期，量子效应是决定性的，在时空结构中产生微小的不均匀性，在随后的宇宙演化中产生大尺度结构。广义相对论与量子力学的一致共轭目标是推动弦理论发展的主要目标。这个理论引入了非常不寻常的概念：它的一致性要求我们的宇宙比观察到的多六个维度，这些维度被包裹在一个小空间中，并且无法通过日常经验观察到。此外，它预测了膜物体的存在，在更高维度的背景中波动，构成我们宇宙的粒子可以被定位。然而，为了验证这些美丽的想法，我们需要探测在极小尺度上发生的现象。我发现所有这些想法都非常令人兴奋，所以我决定研究弦理论和宇宙学之间的关系，主要目的是找到通过宇宙学观测来检验弦理论的新方法。如前所述，在宇宙非常小的早期发生的现象受到短距离物理学的影响，然后可能受到弦论的影响。暴胀是最重要的例子：它是一个在观测到的CMB辐射模式中留下清晰印记的过程，并提供了影响宇宙随后演化的初始条件。由于这些原因，我的部分研究致力于弦理论中的暴胀模型。它们可能具有特殊的性质，因为它们使用了该理论提供的许多成分。因此，对暴胀的弦模型的研究，提供了独特的机会来揭示弦论特有的效应，并允许通过宇宙学观测来检验它的想法。更具体地说，我的研究活动的主要目标可以概括如下。首先，我计划开发理论工具，允许比较观测结果与字符串激励宇宙学模型。这是一个广泛的主题，需要阐述现有的技术，旨在分析宇宙学波动的演变，以便将它们应用到弦激发的宇宙学模型。然后，我将尝试个性化的最有前途的宇宙学模型，基于弦理论，提供了最好的机会被未来的宇宙学观测测试。一旦这样做了，我将试图详细阐述这些模型，以便从理论的角度使它们完全令人满意，并详细研究它们对宇宙学量的预测，这些预测将通过观测来检验。

项目成果

Implications of the Planck bispectrum constraints for the primordial trispectrum

• DOI: 10.1209/0295-5075/103/19001
• 发表时间: 2013-06
• 期刊: Europhysics Letters
• 作者: C. Byrnes;Sami Nurmi;G. Tasinato;D. Wands

Generalised tensor fluctuations and inflation

• DOI: 10.1088/1475-7516/2015/01/029
• 发表时间: 2014-09
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: Dario Cannone;G. Tasinato;D. Wands

EFT beyond the horizon: stochastic inflation and how primordial quantum fluctuations go classical

• DOI: 10.1007/jhep03(2015)090
• 发表时间: 2015-03-18
• 期刊: JOURNAL OF HIGH ENERGY PHYSICS
• 影响因子: 5.4
• 作者: Burgess, C. P.;Holman, R.;Williams, M.
• 通讯作者: Williams, M.

Inhomogeneous non-Gaussianity

• DOI: 10.1088/1475-7516/2012/03/012
• 发表时间: 2011-11
• 期刊: arXiv: Cosmology and Nongalactic Astrophysics
• 作者: C. Byrnes;Sami Nurmi;G. Tasinato;D. Wands

Breaking discrete symmetries in the effective field theory of inflation

• DOI: 10.1088/1475-7516/2015/08/003
• 发表时间: 2015-05
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: Dario Cannone;Jinn-Ouk Gong;G. Tasinato