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arXiv 1006.0486astro-ph.COgr-qchep-phhep-th
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宇宙标准模型中的有效暴胀理论和暗物质地位

The Effective Theory of Inflation and the Dark Matter Status in the Standard Model of the Universe

H. J. de Vega

备注：
28 pages; to be published in the Lev Lipatov Festschrift on the occasion of Lev's 70th birthday, `Subtleties in Quantum Field Theories', D. Diakonov, Editor, Gatchina, Russia, 2010
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摘要：

本文提出了一种类似Ginsburg-Landau的有效暴胀理论，其中暴胀子势是一个多项式。慢滚膨胀变成系统的1/N膨胀，其中N ~ 60。谱指数n_s - 1 = O（1/N），r = O（1/N），而涨落d n_s/d \ln k = O（1/N^2），可以忽略.暴胀的能量标度M ~ 0.7 × 10^{16} GeV完全由标量绝热涨落的振幅决定。一个完整的分析研究加上可用的CMB+LSS数据的蒙特卡罗马尔可夫链（MCMC）分析表明：（a）自发破缺的phi -> - phi对称性的暴胀子潜力。(b)r的下限：r > 0.023（95% CL）和r > 0.046（68% CL）。(c)较好的暴胀势是一个双势阱，偶场函数，具有中等的四次耦合，得到最可几值：n_s = 0.964，r = 0.051。这一r值在CMB即将观测到的范围之内。我们利用宇宙学理论和星系观测研究了DM的性质。我们的DM分析与DM的粒子物理模型无关，它是基于DM相空间密度rho_{DM} /σ ^3_{DM}。我们推导出了DM粒子质量m和退耦时超相对论自由度g_d（即温度）的显式公式。我们发现，m匝是在keV规模。keV尺度DM在结构形成过程中是非相对论性的，它再现了小尺度和大尺度结构，但它不能解释宇宙射线中的e^+和pbar过剩，这可以用天体物理机制来解释（Abridged）。

英文摘要：

We present here the effective theory of inflation `a la Ginsburg-Landau in which the inflaton potential is a polynomial. The slow-roll expansion becomes a systematic 1/N expansion where N ~ 60. The spectral index and the ratio of tensor/scalar fluctuations are n_s - 1 = O(1/N), r = O(1/N) while the running turns to be d n_s/d \ln k = O(1/N^2) and can be neglected. The energy scale of inflation M ~ 0.7 10^{16} GeV is completely determined by the amplitude of the scalar adiabatic fluctuations. A complete analytic study plus the Monte Carlo Markov Chains (MCMC) analysis of the available CMB+LSS data showed: (a) the spontaneous breaking of the phi -> - phi symmetry of the inflaton potential. (b) a lower bound for r: r > 0.023 (95% CL) and r > 0.046 (68% CL). (c) The preferred inflation potential is a double well, even function of the field with a moderate quartic coupling yielding as most probable values: n_s = 0.964, r = 0.051. This value for r is within reach of forthcoming CMB observations. We investigate the DM properties using cosmological theory and the galaxy observations. Our DM analysis is independent of the particle physics model for DM and it is based on the DM phase-space density rho_{DM}/sigma^3_{DM}. We derive explicit formulas for the DM particle mass m and for the number of ultrarelativistic degrees of freedom g_d (hence the temperature) at decoupling. We find that m turns to be at the keV scale. The keV scale DM is non-relativistic during structure formation, reproduces the small and large scale structure but it cannot be responsible of the e^+ and pbar excess in cosmic rays which can be explained by astrophysical mechanisms (Abridged).

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