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A primer on the physics of the cosmic microwave background /
In the last fifteen years, various areas of high energy physics, astrophysics and theoretical physics have converged on the study of cosmology so that any graduate student in these disciplines today needs a reasonably self-contained introduction to the Cosmic Microwave Background (CMB). This book pr...
| Clasificación: | Libro Electrónico |
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| Autor principal: | |
| Formato: | Electrónico eBook |
| Idioma: | Inglés |
| Publicado: |
Singapore ; Hackensack, NJ :
World Scientific,
©2008.
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| Temas: | |
| Acceso en línea: | Texto completo |
Tabla de Contenidos:
- 1. Why CMB physics? 1.1. The blackbody spectrum and its physical implications. 1.2. A bit of history of CMB observations. 1.3. The entropy of the CMB and its implications. 1.4. The time evolution of the CMB temperature. 1.5. A quick glance to the Sunyaev-Zeldovich effect. 1.6. Cosmological parameters
- 2. From CMB to the Standard Cosmological Model. 2.1. The Standard Cosmological Model (SCM). 2.2. Friedmann-Lemaître equations. 2.3. Matter content of the SCM. 2.4. The future of the Universe. 2.5. The past of the Universe. 2.6. Simplified numerical estimates
- 3. Problems with the SCM. 3.1. The horizon problem. 3.2. The spatial curvature problem. 3.3. The entropy problem. 3.4. The structure formation problem. 3.5. The singularity problem
- 4. SCM and beyond. 4.1. The horizon and the flatness problems. 4.2. Classical and quantum fluctuations. 4.3. The entropy problem. 4.4. The problem of geodesic incompleteness
- 5. Essentials of inflationary dynamics. 5.1. Fully inhomogeneous Friedmann-Lemaître equations. 5.2. Homogeneous evolution of a scalar field. 5.3. Classification(s) of inflationary backgrounds. 5.4. Exact inflationary backgrounds. 5.5. Slow-roll dynamics. 5.6. Slow-roll parameters
- 6. Inhomogeneities in FRW models. 6.1. Decomposition of inhomogeneities in FRW Universes. 6.2. Gauge issues for the scalar modes. 6.3. Super-adiabatic amplification. 6.4. Quantum mechanical description of the tensor modes. 6.5. Spectra of relic gravitons. 6.6. Quantum state of cosmological perturbations. 6.7. Digression on different vacua. 6.8. Numerical estimates of the mixing coefficients
- 7. The first lap in CMB anisotropies. 7.1. Tensor Sachs-Wolfe effect. 7.2. Scalar Sachs-Wolfe effect. 7.3. Scalar modes in the pre-decoupling phase. 7.4. CDM-radiation system. 7.5. Adiabatic and non-adiabatic modes: an example. 7.6. Sachs-Wolfe plateau: mixture of initial conditions
- 8. Improved fluid description of pre-decoupling physics. 8.1. The general plasma with four components. 8.2. CDM component. 8.3. Tight-coupling between photons and baryons. 8.4. Shear viscosity and silk damping. 8.5. The adiabatic solution. 8.6. Pre-equality non-adiabatic initial conditions. 8.7. Numerics in the tight-coupling approximation
- 9. Kinetic hierarchies. 9.1. Collisionless Boltzmann equation. 9.2. Boltzmann hierarchy for massless neutrinos. 9.3. Brightness perturbations of the radiation field. 9.4. Evolution equations for the brightness perturbations. 9.5. Line of sight integrals. 9.6. Tight-coupling expansion. 9.7. Zeroth order in tight-coupling: acoustic oscillations. 9.8. First order in tight-coupling: polarization. 9.9. Second order in tight-coupling: diffusion damping. 9.10. Semi-analytical approach to Doppler oscillations
- 10. Early initial conditions? 10.1. Minimally coupled scalar field. 10.2. Spectral relations. 10.3. Curvature perturbations and density contrasts. 10.4. Hamiltonians for the scalar problem. 10.5. Trans-Planckian problems? 10.6. How many adiabatic modes?
- 11. Surfing on the gauges. 11.1. The longitudinal gauge. 11.2. The synchronous gauge. 11.3. Comoving orthogonal hypersurfaces. 11.4. Uniform density hypersurfaces. 11.5. The off-diagonal gauge. 11.6. Mixed gauge-invariant treatments
- 12. Interacting fluids. 12.1. Interacting fluids with bulk viscous stresses. 12.2. Evolution equations for the entropy fluctuations. 12.3. Specific physical limits. 12.4. Mixing between entropy and curvature perturbations
- 13. Spectator fields. 13.1. Spectator fields in a fluid background. 13.2. Unconventional inflationary models. 13.3. Conventional inflationary models.