暴涨宇宙学与暗能量 - Center for High Energy Physics, Tsinghua.PPT

需要新物理 暗物质：中微子是暗物质，但不是冷暗物质；什么是冷暗物质？ 暗能量：势能和真空能是暗能量，但理论预言太大－宇宙学常数问题？ 反物质：标准模型可以产生正反物质不对称，但太小，需要新物理？ Inflation：什么是inflaton？ Application showcase: neutrino mass Weighing neutrinos in the presence of a running primordial spectral indexastro-ph/0605742 Bo Feng, Jun-Qing Xia, Junichi Yokoyama, Xinmin Zhang, Gong-Bo ZhaoThe three-year WMAP(WMAP3), combined with other cosmological observations from galaxy clustering and Type Ia Supernova (SNIa), prefers a non-vanishing running of the primordial spectral index independent of the low CMB multipoles. Motivated by this feature we study cosmological constraint on the neutrino mass, which severely depends on what prior we adopt for the spectral shape of primordial fluctuations, taking possible running into account. As a result we find a more stringent constraint on the sum of the three neutrino masses, m_\nu 0.76 eV (2 \sigma), compared with the case where power-law prior is adopted to the primordial spectral shape. Cosmic rays from the halo of the MW—some weak hints on DM Some astrophysics observations can not be explained by the canonical physics. They may indicate the signal of DM, however, no conclusion can be drawn now. One of such experiments is the HEAT. (The HEAT signal may indicate the non-thermal production or the subhalo nearby) Constraints on EOS from SN Ia 暗能量参数化： I. 一个常数 w II. 动力学参数化 a. b. 利用 SN Ia 数据限模型 Global fitting with SN Ia, galaxy clustering and WMAP3 Quintom is also mildly favored The standard ΛCDM model is still a good fit to the current data 暗能量研究现状小结 宇宙学常数可以自洽的拟合数据 动力学暗能量（Quintessence, Phantom, Quintom………）没有被排除 Quintom is mildly favored 中微子振荡检验暗能量 D.B. Kaplan et al., PRL 93,091801 (2003); V. Barger et al., PRL 95 (2005) 211802; M. Cirelli et al., NPB 719 219 (2005). Searching For CPT Violation With WMAP And BOOMERANGastro-ph/0601095 Bo Feng, Mingzhe Li, Jun-Qing Xia, Xuelei Chen, Xinmin ZhangVersion accepted by PRL We search for signatur