| 书目名称 | Theoretical and Observational Cosmology | | 编辑 | Marc Lachièze-Rey | | 视频video | | | 丛书名称 | Nato Science Series C: | | 图书封面 |  | | 描述 | A complete account of the fundamental techniques of generalrelativity and their application to cosmology. The book includesreviews of the different cosmological models and their classification,including such topics as causality and horizons, the cosmologicalparameters, observational tests and constraints of cosmology,symmetries and the large scale topology of space and space-time, andthe use of supernovas as cosmological indicators. .The perturbations to the cosmological models are discussed throughoutthe volume. The cosmic microwave background is presented, with anemphasis in secondary distortions in relation to cosmological modelsand large scale structures. Recent results on dark matter aresummarised. A general review of primordial nucleosynthesis is given.Gravitational lensing is discussed in great detail. Most contributionsshow a balance between theory and observation. ..Readership.: A solid background for students and researchersintending to work in the field of theoretical and observationalcosmology. | | 出版日期 | Book 1999 | | 关键词 | Cosmology; Dark matter; Gravity; Redshift; Relativity; Universe; general relativity | | 版次 | 1 | | doi | https://doi.org/10.1007/978-94-011-4455-1 | | isbn_softcover | 978-0-7923-5946-3 | | isbn_ebook | 978-94-011-4455-1Series ISSN 1389-2185 | | issn_series | 1389-2185 | | copyright | Springer Science+Business Media Dordrecht 1999 |
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,Cosmological Models, |
George F. R. Ellis,Henk Van Elst |
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Abstract
The aim of this set of lectures is a systematic presentation of a 1 + 3 covariant approach to studying the geometry, dynamics, and observational properties of relativistic cosmological models. In giving (i) the basic 1+ 3 covariant relations for a cosmological fluid, the present lectures cover some of the same ground as a previous set of Cargèse lectures [.], but they then go on to give (ii) the full set of corresponding tetrad equations, (iii) a classification of cosmological models with exact symmetries, (iv) a brief discussion of some of the most useful exact models and their observational properties, and (v) an introduction to the gauge-invariant and 1 + 3 covariant perturbation theory of almost-Friedmann—LemaîtreRobertson—Walker universes, with a fluid description for the matter and a kinetic theory description of the radiation.
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,Topology of the Universe: Theory and Observation, |
Jean-Pierre Luminet,Boudewijn F. Roukema |
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Abstract
“One could imagine that as a result of enormously extended astronomical experience, the entire universe consists of countless identical copies of our Milky Way, that the infinite space can be partitioned into cubes each containing an exactly identical copy of our Milky Way. Would we really cling on to the assumption of infinitely many identical repetitions of the same world?… We would be much happier with the view that these repetitions are illusory, that in reality space has peculiar connection properties so that if we leave any one cube through a side, then we immediately reenter it through the opposite side.” (..).Developments in the theoretical and observational sides of cosmic topology were slow for most of the century, but are now progressing rapidly at a scale of most interest, with the hope of detecting the topological parameters of the universe within the next ten years..The historical, mathematical and observational aspects of the subject are briefly reviewed in this course.
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,Symmetries in General Relativity and Beyond, |
M. Lachièze-Rey |
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Abstract
All past, present and prospective physical theories are expressed in (three dimensional) space or (four dimensional) space-time, which appear as the frame to describe physical events. Although fundamental, the concepts of space and space-time strongly differ in different theories, in particular in quantum physics and general relativity. Moreover, the tendencies of contemporary research may involve still different concepts (different number of dimensions, discreteness,…).
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| 1 |
,Gravitational Lenses, |
Francis Bernardeau |
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Abstract
Gravitational lenses are becoming a precious mean of probing the matter distribution in the Universe. From the search of matter in the Galactic halo to the study of the large-scale structures of the Universe, the gravitational lens effects offer a unique alternative to light surveys and are now widely used. This evolution is due in particular to the use of new observation devices, such as the wide field CCD cameras.
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,Cosmological Applications of Gravitational Lensing, |
Y. Mellier |
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Abstract
Because gravitational lensing provides a unique tool to probe almost directly the dark matter, its use for cosmology is of considerable interest. The discovery of giant arc(let)s in clusters of galaxies (., ., .) or Einstein rings around galaxies (.), and the spectroscopic proofs that they are produced by gravitational lensing effects (.) have revealed that gravitational distortion can probe with a remarkable amount of details the mass distribution of clusters (., .) and galaxies (.).
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,Measurement of Cosmological Parameters Using Type Ia Supernovae, |
R. Pain |
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Abstract
In this lecture, I present the method used to measure the cosmological parameters using type la supernovae (SNe Ia) in section 1 and discuss SNe la as cosmological tools in section 2. The detection and follow-up of highredshift supernovae is presented in section 3 and in section 4, recent results on the measurement of Ho, S2M and QA are reported. Prospects for the near future are briefly discussed in section 5.
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,Primordial Nucleosynthesis, |
K. A. Olive |
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Abstract
Big Bang Nucleosynthesis (BBN) is the theory explaining the origins of the light elements D,.He, .He, and .Li and their primordial abundances. The theoretical framework for BBN is quite simple. It is based on FriedmannLemaitre-Robertson-Walker cosmology [.] and a network of nuclear reactions. We can further specify that the standard BBN model refers to homogeneous nucleosynthesis in the context of a FLRW Universe with an electroweak standard model particle content, which for the purposes of BBN really amounts to assuming the existence of three nearly massless and nearly stable neutrinos. The predictions of BBN for the abundances of the light elements are determined by running a code which incorporates the nuclear network in a thermal (and cooling due to the expansion of the Universe) bath. These predictions are then be compared with the observational determinations of the abundances.
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,Searches for Dark Matter, |
J. Rich |
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Abstract
There appears to be an emerging consensus (e.g. (.)) that the Universe consists primarily of non-baryonic dark matter (~ 0.3 critical density) and an effective vacuum energy density (~ 0.7 critical density). Evidence for this mixture is highly indirect. It comes from combining data on the clustering properties of galaxies, on the anisotropies of the cosmic background radiation, and on the redshift-magnitude diagram of type Ia supernovae (.;.;.).
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,Temperature Anisotropies of the Cosmic Microwave Background, |
N. Aghanim |
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Abstract
The Cosmic Microwave Background (CMB), discovered in 1965 by Penzias and Wilson (Penzias Sz Wilson 1965), is one of the main observational tools for cosmology. It is characterised by:
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,Primordial Galaxies: From Local HII Galaxies to High Redshift Galaxies, |
D. Kunth |
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Abstract
Primordial galaxies at early epoch may be strong Lya emitters. I review the results of recent studies of local . galaxies on their Lya emission that are relevant to the search of distant young galaxies. The interdependance of the Lya escape with the properties of the ISM in starburst galaxies is outlined. A new model explains Lya profiles in starburst galaxies from the hydrodynamics of superbubbles powered by massive stars. Since Lya is primarely a diagnostic of the ISM, it is mandatory to understand how the ISM and Lya are related to firmly relate Lya to the cosmic star-formation rate. Lya search of distant dust-free young galaxies is now a reachable possibility.
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,Active Galactic Nuclei, |
Guy Mathez |
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Abstract
In what is defined as Active Galactic Nuclei, the stellar contribution to the emitted light is generally less than (or exceptionally equal to) half the total emitted power. Even if a spectrum of an active galaxy was taken as early as 1908, Seyfert was the first astronomer to understand that.do form a class. Seyfert’s original work (1943) listed 12 galaxies, defined at that time as.Spectroscopy then revealed most characteristic properties of Seyfert galaxies, the standard of AGN: a.(with respect to usual galaxy continua), together with numerous broad emission lines with high degree of ionization and excitation. Other characteristics of AGN are the following: they have in average large redshifts, some are radio loud, almost all are X-ray emitters, a majority seems to emit in the high-energy range, γ-ray and TeV bands, and many of them present time variability. The discrimination between active galaxies and quasars is mostly historical, due to the very different morphologies of the first Seyferts and quasars. Furthermore, the status of AGN remained unclear for a long time, due to the mixture of morphological and spectroscopic criteria used in many of their first classifications. Since that time, and essentially based on the similarity of their spectra and of most of their properties which vary continuously from the low luminosity less active galaxies to the most luminous quasars.
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,Cosmic Velocity Fields, |
J. F. L. Simmons |
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Abstract
The velocity of the Local Group with respect to the CMBR has been determined to be about 600 km s.. A significant difference between the actual direction of motion and the direction to the nearest large cluster of galaxies, the Virgo cluster, led astronomers to believe in the existence of a mass concentration beyond, the so called Great Attractor, and to recognise the importance of large scale bulk motions.
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发表于 2025-3-21 19:15:56
