arXiv 0709.29122007-09astro-phhep-phhep-th

耗散暴胀模型的宇宙学约束

Cosmological Constraints on Dissipative Models of Inflation

Lisa M. H. Hall, Hiranya V. Peiris

备注：: 14 pages, 9 figures, Accepted by JCAP without text changes, References added
发表信息：: JCAP 0801:027,2008
DOI：: 10.1088/1475-7516/2008/01/027

摘要：

我们研究了耗散项具有特定形式的区域中的耗散暴胀，分析了具有超对称破缺势的弱耗散区域和强耗散区域中的两个模型.在通过解析近似对这些模型的预测发展直觉之后，我们通过运动方程的完全数值演化计算预测的宇宙学观测值，将质量尺度和耗散尺度与原始功率谱的特征振幅和形状联系起来。然后，我们使用马尔可夫链蒙特卡罗技术约束的一个子集的模型与宇宙学数据的宇宙微波背景（WMAP三年的数据）和大尺度结构（SDSS发光的红色星系功率谱）。我们发现，耗散参数的后验分布是高度非高斯和他们的允许范围同意以及使用解析近似得到的期望。在弱区，只有质量尺度受到严格约束;相反，在强区，只有耗散系数受到严格约束。暴胀尺度上有一个下限：次普朗克暴胀不受数据的青睐。在弱和强的制度，我们重建的原始功率谱的限制，并表明这些模型更喜欢{ \it红色}频谱，没有显着的运行的指数。我们计算的再热温度，并表明，引力子问题可以克服与大耗散，这反过来又导致大的非高斯性水平：如果耗散膨胀是为了逃避引力子问题，预测的非高斯性水平可能会被普朗克卫星。

英文摘要：

(Abridged) We study dissipative inflation in the regime where the dissipative term takes a specific form, Γ=Γ(ϕ), analyzing two models in the weak and strong dissipative regimes with a SUSY breaking potential. After developing intuition about the predictions from these models through analytic approximations, we compute the predicted cosmological observables through full numerical evolution of the equations of motion, relating the mass scale and scale of dissipation to the characteristic amplitude and shape of the primordial power spectrum. We then use Markov Chain Monte Carlo techniques to constrain a subset of the models with cosmological data from the cosmic microwave background (WMAP three-year data) and large scale structure (SDSS Luminous Red Galaxy power spectrum). We find that the posterior distributions of the dissipative parameters are highly non-Gaussian and their allowed ranges agree well with the expectations obtained using analytic approximations. In the weak regime, only the mass scale is tightly constrained; conversely, in the strong regime, only the dissipative coefficient is tightly constrained. A lower limit is seen on the inflation scale: a sub-Planckian inflaton is disfavoured by the data. In both weak and strong regimes, we reconstruct the limits on the primordial power spectrum and show that these models prefer a {\it red} spectrum, with no significant running of the index. We calculate the reheat temperature and show that the gravitino problem can be overcome with large dissipation, which in turn leads to large levels of non-Gaussianity: if dissipative inflation is to evade the gravitino problem, the predicted level of non-Gaussianity might be seen by the Planck satellite.

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