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...
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| Format: | Elektronisch E-Book |
| Sprache: | English |
| Veröffentlicht: |
Singapore ; Hackensack, NJ :
World Scientific,
©2008.
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| Schlagworte: | |
| Online-Zugang: | Volltext |
| Zusammenfassung: | 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 presents the essential theoretical tools necessary to acquire a modern working knowledge of CMB physics. The style of the book, falling somewhere between a monograph and a set of lecture notes, is pedagogical and the author uses the typical approach of theoretical physics to explain the main problems in detail, touching on the main assumptions and derivations of a fascinating subject. |
| Beschreibung: | 1 online resource (xiv, 474 pages) : illustrations |
| Bibliographie: | Includes bibliographical references (pages 455-466) and index. |
| ISBN: | 9789812791436 9812791434 1281933937 9781281933935 9786611933937 661193393X |
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| 245 | 1 | 2 | |a A primer on the physics of the cosmic microwave background / |c Massimo Giovannini. |
| 260 | |a Singapore ; |a Hackensack, NJ : |b World Scientific, |c ©2008. | ||
| 300 | |a 1 online resource (xiv, 474 pages) : |b illustrations | ||
| 336 | |a text |b txt |2 rdacontent | ||
| 337 | |a computer |b c |2 rdamedia | ||
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| 504 | |a Includes bibliographical references (pages 455-466) and index. | ||
| 505 | 0 | |a 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. | |
| 520 | |a 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 presents the essential theoretical tools necessary to acquire a modern working knowledge of CMB physics. The style of the book, falling somewhere between a monograph and a set of lecture notes, is pedagogical and the author uses the typical approach of theoretical physics to explain the main problems in detail, touching on the main assumptions and derivations of a fascinating subject. | ||
| 588 | 0 | |a Print version record. | |
| 546 | |a English. | ||
| 650 | 0 | |a Cosmic background radiation. |0 http://id.loc.gov/authorities/subjects/sh88007683 | |
| 650 | 0 | |a Physics. |0 http://id.loc.gov/authorities/subjects/sh85101653 | |
| 650 | 2 | |a Physics |0 https://id.nlm.nih.gov/mesh/D010825 | |
| 650 | 6 | |a Rayonnement cosmologique. | |
| 650 | 6 | |a Physique. | |
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| 650 | 7 | |a Cosmic background radiation |2 fast | |
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| contents | 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. |
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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. 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| illustrated | Illustrated |
| indexdate | 2024-11-27T13:16:43Z |
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| spelling | Giovannini, Massimo, 1968- https://id.oclc.org/worldcat/entity/E39PCjrx7X6mbqpxT7phKKJGgX http://id.loc.gov/authorities/names/no2008094039 A primer on the physics of the cosmic microwave background / Massimo Giovannini. Singapore ; Hackensack, NJ : World Scientific, ©2008. 1 online resource (xiv, 474 pages) : illustrations text txt rdacontent computer c rdamedia online resource cr rdacarrier Includes bibliographical references (pages 455-466) and index. 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. 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 presents the essential theoretical tools necessary to acquire a modern working knowledge of CMB physics. The style of the book, falling somewhere between a monograph and a set of lecture notes, is pedagogical and the author uses the typical approach of theoretical physics to explain the main problems in detail, touching on the main assumptions and derivations of a fascinating subject. Print version record. English. Cosmic background radiation. http://id.loc.gov/authorities/subjects/sh88007683 Physics. http://id.loc.gov/authorities/subjects/sh85101653 Physics https://id.nlm.nih.gov/mesh/D010825 Rayonnement cosmologique. Physique. physics. aat SCIENCE Cosmology. bisacsh Physics fast Cosmic background radiation fast has work: A primer on the physics of the cosmic microwave background (Text) https://id.oclc.org/worldcat/entity/E39PCFyRPBJ4QYPk7dxgPKMByd https://id.oclc.org/worldcat/ontology/hasWork Print version: Giovannini, Massimo, 1968- Primer on the physics of the cosmic microwave background. Singapore ; Hackensack, NJ : World Scientific, ©2008 9812791426 9789812791429 (DLC) 2008299029 (OCoLC)191658608 FWS01 ZDB-4-EBA FWS_PDA_EBA https://search.ebscohost.com/login.aspx?direct=true&scope=site&db=nlebk&AN=236097 Volltext |
| spellingShingle | Giovannini, Massimo, 1968- A primer on the physics of the cosmic microwave background / 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. Cosmic background radiation. http://id.loc.gov/authorities/subjects/sh88007683 Physics. http://id.loc.gov/authorities/subjects/sh85101653 Physics https://id.nlm.nih.gov/mesh/D010825 Rayonnement cosmologique. Physique. physics. aat SCIENCE Cosmology. bisacsh Physics fast Cosmic background radiation fast |
| subject_GND | http://id.loc.gov/authorities/subjects/sh88007683 http://id.loc.gov/authorities/subjects/sh85101653 https://id.nlm.nih.gov/mesh/D010825 |
| title | A primer on the physics of the cosmic microwave background / |
| title_auth | A primer on the physics of the cosmic microwave background / |
| title_exact_search | A primer on the physics of the cosmic microwave background / |
| title_full | A primer on the physics of the cosmic microwave background / Massimo Giovannini. |
| title_fullStr | A primer on the physics of the cosmic microwave background / Massimo Giovannini. |
| title_full_unstemmed | A primer on the physics of the cosmic microwave background / Massimo Giovannini. |
| title_short | A primer on the physics of the cosmic microwave background / |
| title_sort | primer on the physics of the cosmic microwave background |
| topic | Cosmic background radiation. http://id.loc.gov/authorities/subjects/sh88007683 Physics. http://id.loc.gov/authorities/subjects/sh85101653 Physics https://id.nlm.nih.gov/mesh/D010825 Rayonnement cosmologique. Physique. physics. aat SCIENCE Cosmology. bisacsh Physics fast Cosmic background radiation fast |
| topic_facet | Cosmic background radiation. Physics. Physics Rayonnement cosmologique. Physique. physics. SCIENCE Cosmology. Cosmic background radiation |
| url | https://search.ebscohost.com/login.aspx?direct=true&scope=site&db=nlebk&AN=236097 |
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