第二讲 宇宙微波背景辐射

简单介绍了近年来关于宇宙微波背景辐射在观测上取得的重大进展,以及有关它的解释、理论和意义.宇宙微波背景是我们了解宇宙奥秘的一个至关重要的窗口.在未来几年,它还将扮演更加重要的角色.     

第二讲宇宙微波背景辐射

简单介绍了近年来关于宇宙微波背景辐射在观测上取得的重大进展，以及有关它的解释、理论和意义．宇宙微波背景是我们了解宇宙奥秘的一个至关重要的窗口．在未来几年，它还将扮演更加重要的角色．     

Cosmic spinor fields and the early universe

The energy production through expansion of the universe is studied for the Dirac spinor field in all three types of Robertson-Walker universes. Only in the open case is the matter production unlimited (closed universe: limited; flat universe: impossible). The physical properties of the cosmological solutions to the Dirac equation over any RW background are studied in detail.     

Cosmic microwave background spectrum and G-varying cosmology

It is shown that G-varying cosmologies provide a better fit to the observed data on cosmic microwave background, than the standard Friedmann models.     

Cosmic microwave background radiation anisotropies in brane worlds

We propose a new formulation to calculate the cosmic microwave background (CMB) spectrum in the Randall-Sundrum two-brane model based on recent progress in solving the bulk geometry using a low energy approximation. The evolution of the anisotropic stress imprinted on the brane by the 5D Weyl tensor is calculated. An impact of the dark radiation perturbation on the CMB spectrum is investigated in a simple model assuming an initially scale-invariant adiabatic perturbation. The dark radiation perturbation induces isocurvature perturbations, but the resultant spectrum can be quite different from the prediction of simple mixtures of adiabatic and isocurvature perturbations due to Weyl anisotropic stress.     

Cosmic microwave background radiation anisotropies and data analysis

The theory of generation of CMBR temperature and polarization fluctuations is briefly reviewed. Also discussed is the present status of observations and the nature of future surveys.     

The cosmic microwave background and the hadron era of the early universe: A possible connection

A cosmological model is constructed which is a Friedman model, but with a finite ultimate temperature (T_F). A plausible argument is presented which suggests that the existence of T_F and the cosmic microwave background restricts the form of the hadronic level density:

, where A, B = constants. In our model, $\text{B =}\text{7}\text{2}\text{?}\text{3}\text{s}\text{,}\text{where}\text{s =}\text{positive}$ integer. The case $\text{s = 3 (B =}\text{5}\text{2}\text{)}$ is the well-known Hagedorn model; the Frautschi model corresponds to s = 6 (B = 3); the cases $\text{s = 1 (B =}\text{1}\text{2}\text{)}$ and s = 2 (B = 2) have not been considered before now. For each value of $\text{B <}\text{7}\text{2}$, the model gives the temperature (T_γ0) of the microwave background as a function of A, T_F and ?₀ (the present energy density of the universe). Two fascinating results then emerge: first, all estimates of T_γ0 favor a low density Friedman universe (?0 = 10^?31g/cm³), which rules out a universe with positive curvature; second, for ?₀ = 10^?31gr/cm³ the best estimate of T_γ0 (?3K) occurs for the Hagedorn model.     

Cosmic infrared background and early galaxy evolution

The cosmic infrared background (CIB) reflects the sum total of galactic luminosities integrated over the entire age of the universe. From its measurement the red-shifted starlight and dust-absorbed and re-radiated starlight of the CIB can be used to determine (or constrain) the rates of star formation and metal production as a function of time and deduce information about objects at epochs currently inaccessible to telescopic studies. This review discusses the state of current CIB measurements and the (mostly space-based) instruments with which these measurements have been made, the obstacles (the various foreground emissions) and the physics behind the CIB and its structure. Theoretical discussion of the CIB levels can now be normalized to the standard cosmological model narrowing down theoretical uncertainties. We review the information behind and theoretical modeling of both the mean (isotropic) levels of the CIB and their fluctuations. The CIB is divided into three broad bands: near-IR (NIR), mid-IR (MIR) and far-IR (FIR). For each of the bands we review the main contributors to the CIB flux and the epochs at which the bulk of the flux originates. We also discuss the data on the various quantities relevant for correct interpretation of the CIB levels: the star-formation history, the present-day luminosity function measurements, resolving the various galaxy contributors to the CIB, etc. The integrated light of all galaxies in the deepest NIR galaxy counts to date fails to match the observed mean level of the CIB, probably indicating a significant high-redshift contribution to the CIB. Additionally, Population III stars should have left a strong and measurable signature via their contribution to the CIB anisotropies for a wide range of their formation scenarios, and measuring the excess CIB anisotropies coming from high z would provide direct information on the epoch of the first stars.     

Cosmic microwave background anisotropy constraints on relict neutrinos

I discuss basic theory of effect of the properties of the cosmological relict neutrinos on the observations of the cosmic microwave background anisotropy.     

Hawking process and the cosmic microwave background in a steady state universe

It is investigated whether a large number of primordial black holes can account for the observed microwave background in a steady state universe. The answer is shown to be negative.     

Ellipsoidal universe can solve the cosmic microwave background quadrupole problem

The recent 3 yr Wilkinson Microwave Anisotropy Probe data have confirmed the anomaly concerning the low quadrupole amplitude compared to the best-fit Lambda-cold dark matter prediction. We show that by allowing the large-scale spatial geometry of our universe to be plane symmetric with eccentricity at decoupling or order 10(-2), the quadrupole amplitude can be drastically reduced without affecting higher multipoles of the angular power spectrum of the temperature anisotropy.