標(biāo)題: Titlebook: Galaxy Formation; Malcolm S. Longair Textbook 19981st edition The Editor(s) (if applicable) and The Author(s), under exclusive license to [打印本頁(yè)] 作者: genial 時(shí)間: 2025-3-21 18:06
書(shū)目名稱(chēng)Galaxy Formation影響因子(影響力)
作者: 噴油井 時(shí)間: 2025-3-21 21:25 作者: outer-ear 時(shí)間: 2025-3-22 03:10
Textbook 19981st editioneveryone‘s needs?‘ I was asked by Springer-Verlag to expand into a full-length book the set of lecture notes that I prepared in 1988 for the First Astrophysics School organised by the European Astrophysics Doctoral Network. The set of notes was entitled Galaxy Formation and was published as a chapte作者: deviate 時(shí)間: 2025-3-22 06:49
Liquid Scintillation Counting of Tritiumtus of General Relativity is surveyed and it is shown that it is the best relativistic theory of gravity we possess. If you are happy to accept General Relativity at its face value, you may advance to Chap. 7.作者: NICHE 時(shí)間: 2025-3-22 08:49
Advances in Transplant Dermatologyluid moves along streamlines in the universal expansion and so behaves like a perfect fluid for which the energy—momentum tensor is given by the ... of (6.30); ? General Relativity, which enables us to relate the energy—momentum tensor to the geometrical properties of space-time through (6.43) or (6.44).作者: 他日關(guān)稅重重 時(shí)間: 2025-3-22 15:57 作者: 他日關(guān)稅重重 時(shí)間: 2025-3-22 17:09 作者: 確定無(wú)疑 時(shí)間: 2025-3-22 22:37
The Friedman World Modelsluid moves along streamlines in the universal expansion and so behaves like a perfect fluid for which the energy—momentum tensor is given by the ... of (6.30); ? General Relativity, which enables us to relate the energy—momentum tensor to the geometrical properties of space-time through (6.43) or (6.44).作者: Flu表流動(dòng) 時(shí)間: 2025-3-23 05:01
Fluctuations in the Cosmic Microwave Background Radiationn it changed from being a fully ionised plasma to a neutral gas. We have dealt with a number of important aspects of the physics of this process in Sect. 9.3, but now we need to understand these in a little more detail.作者: 仔細(xì)檢查 時(shí)間: 2025-3-23 05:59
0941-7834 uite enough books on cosmology to satisfy everyone‘s needs?‘ I was asked by Springer-Verlag to expand into a full-length book the set of lecture notes that I prepared in 1988 for the First Astrophysics School organised by the European Astrophysics Doctoral Network. The set of notes was entitled Gala作者: 顯赫的人 時(shí)間: 2025-3-23 10:52 作者: 模仿 時(shí)間: 2025-3-23 17:48
The Thermal History of the Universe work out the thermal history of the matter and radiation content of the standard Big Bang picture. In this and the succeeding Chap. 10, we will develop many concepts which are essential for understanding the problems of galaxy formation. Let us first consider the dynamics of radiation-dominated universes.作者: STALL 時(shí)間: 2025-3-23 18:53
Hans-Hermann Fernholz,Heinrich E. Fiedlerutrinos provide an example of the decoupling processes which may be important for other unknown types of weakly interacting particle. We will find a qualitatively similar example when we study possible forms of the dark matter.作者: 古董 時(shí)間: 2025-3-24 01:24
B. Kadoch,W. J. T. Bos,K. SchneiderUniverse must be in some non-baryonic form. We need to convince ourselves of the reasoning behind this dramatic conclusion — the nature of the non-baryonic dark matter is of fundamental importance for physics and cosmology.作者: conduct 時(shí)間: 2025-3-24 02:57
Nucleosynthesis in the Early Universeutrinos provide an example of the decoupling processes which may be important for other unknown types of weakly interacting particle. We will find a qualitatively similar example when we study possible forms of the dark matter.作者: Monolithic 時(shí)間: 2025-3-24 07:57
The Simplest Picture of Galaxy Formation and Why It FailsUniverse must be in some non-baryonic form. We need to convince ourselves of the reasoning behind this dramatic conclusion — the nature of the non-baryonic dark matter is of fundamental importance for physics and cosmology.作者: overwrought 時(shí)間: 2025-3-24 11:09 作者: ACRID 時(shí)間: 2025-3-24 16:28
Galaxiesared with, say, the physics of the stars..This is an enormous subject and we will only touch on some of the more important aspects of galaxies, as well as elucidating some of the essential physics. In the next chapter, we will perform a similar exercise for clusters of galaxies.作者: 有助于 時(shí)間: 2025-3-24 20:48
Clusters of Galaxiesonment. Interactions of galaxies with each other and with the intergalactic medium in the cluster can be studied, as well as the distribution and nature of the dark matter, which dominates their dynamics. These are key topics for the physics of galaxy formation.作者: 增強(qiáng) 時(shí)間: 2025-3-25 01:54
The Theoretical Frameworkretation of the space and time coordinates to be used in these calculations. For example, de Sitter’s solution for an empty universe could be written in apparently stationary form, or as an exponentially expanding solution. By 1935, the problem was solved independently by Robertson and Walker. They 作者: 神圣將軍 時(shí)間: 2025-3-25 04:11 作者: pessimism 時(shí)間: 2025-3-25 08:31 作者: 專(zhuān)心 時(shí)間: 2025-3-25 12:35 作者: Epithelium 時(shí)間: 2025-3-25 16:02 作者: institute 時(shí)間: 2025-3-25 23:49
Introduction, History and Outlinehis chapter summarises qualitatively many of the topics dealt with in this book and we will return to all of them in the succeeding chapters. If you do not need this gentle introduction, or misguidedly think that history is boring, you may pass straightaway to Chap. 2..作者: 避開(kāi) 時(shí)間: 2025-3-26 01:24
The Large Scale Structure of the Universeobservation. In this chapter, we concentrate upon the large-scale distribution of matter and radiation in the Universe and deal with galaxies and clusters of galaxies in Chaps. 3 and 4 respectively. The observations described in this chapter provide much of the essential underpinning of modern cosmo作者: 壕溝 時(shí)間: 2025-3-26 04:26 作者: 錯(cuò) 時(shí)間: 2025-3-26 08:28
Clusters of Galaxiestures on scales much greater than clusters, the vast ‘walls’ which surround the large voids seen in Fig. 2.5. Very few galaxies can be considered to be truly isolated. Rich clusters of galaxies are of particular interest because they are the largest gravitationally bound systems we know of in the Un作者: 阻擋 時(shí)間: 2025-3-26 15:03 作者: fringe 時(shí)間: 2025-3-26 17:00 作者: JEER 時(shí)間: 2025-3-26 23:14
The Friedman World Models constructed. The standard models contain three essential ingredients: ? The ., which, combined with the observations that the Universe is isotropic, homogeneous and uniformly expanding on a large scale, leads to the Robertson—Walker metric (5.36); ., according to which the world lines of particles 作者: 食料 時(shí)間: 2025-3-27 04:17 作者: squander 時(shí)間: 2025-3-27 07:56
Nucleosynthesis in the Early Universelight elements by . which took place during the first 10 minutes of our Universe. The results of this analysis are crucial for a number of aspects of galaxy formation. In particular, primordial nucleosynthesis provides one of the most important constraints upon the density parameter in the form of b作者: Oration 時(shí)間: 2025-3-27 12:54 作者: 冷峻 時(shí)間: 2025-3-27 17:33
The Simplest Picture of Galaxy Formation and Why It Failser, we examine the case in which it is assumed that all the matter in the Universe, both ‘visible’ and dark, is in baryonic form. This was the natural starting point for the first plausible models for galaxy formation in the 1960s and 1970s, but they are doomed to failure. Despite this, there are tw作者: 我還要背著他 時(shí)間: 2025-3-27 18:40
Correlation Functions and the Spectrum of the Initial Fluctuationsmake assumptions about the spectrum of the fluctuations from which galaxies and larger scale structures formed. The natural way of describing the distribution of galaxies on the large scale is in terms of . and their associated .. The objective is to relate these properties of the distribution of ga作者: PHIL 時(shí)間: 2025-3-28 01:47
Fluctuations in the Cosmic Microwave Background Radiationonting theories of the origin of the large-scale structure of the Universe with observation. The problem addressed in this chapter is how to relate the fluctuations in the dark and baryonic matter on the last scattering surface at the epoch of recombination to the intensity fluctuations which they i作者: 馬具 時(shí)間: 2025-3-28 06:09 作者: 使高興 時(shí)間: 2025-3-28 08:10 作者: 內(nèi)疚 時(shí)間: 2025-3-28 12:24 作者: 名詞 時(shí)間: 2025-3-28 15:48
Eva B. Griepp,Randall B. GrieppLet us recall the reasons for taking dark matter, and in particular non-baryonic dark matter, very seriously in the context of galaxy formation.作者: 常到 時(shí)間: 2025-3-28 20:14 作者: 轉(zhuǎn)折點(diǎn) 時(shí)間: 2025-3-28 23:42
Dark Matter and Galaxy FormationLet us recall the reasons for taking dark matter, and in particular non-baryonic dark matter, very seriously in the context of galaxy formation.作者: cognizant 時(shí)間: 2025-3-29 03:52
Malcolm S. LongairExcellently suited as a textbook作者: 中和 時(shí)間: 2025-3-29 08:38 作者: 相互影響 時(shí)間: 2025-3-29 14:20
Norsiah Kadir,Mohd Zaini Abd Karimobservation. In this chapter, we concentrate upon the large-scale distribution of matter and radiation in the Universe and deal with galaxies and clusters of galaxies in Chaps. 3 and 4 respectively. The observations described in this chapter provide much of the essential underpinning of modern cosmo作者: Frequency 時(shí)間: 2025-3-29 18:29
Stephanie Ling Jie Lee,Sijie LinUnfortunately, the astrophysics of normal galaxies is only partially under?stood and many important questions remain unresolved. Part of the problem arises from the fact that galaxies are complex, many-body systems. Typically, a galaxy consists of hundreds of millions or billions of stars, it can co作者: 談判 時(shí)間: 2025-3-29 22:04
K. Schmid,H. Fürer,G. D?ndlikertures on scales much greater than clusters, the vast ‘walls’ which surround the large voids seen in Fig. 2.5. Very few galaxies can be considered to be truly isolated. Rich clusters of galaxies are of particular interest because they are the largest gravitationally bound systems we know of in the Un作者: 施魔法 時(shí)間: 2025-3-30 01:48
M. A. Muhs,E. L. Bastin,B. E. Gordont the Universe is isotropic, homogeneous and expanding uniformly at the present epoch. In other words, we smooth out all the finescale structure in the Universe. It is intriguing that this is precisely what Einstein assumed in his static model of 1917, the first fully selfconsistent model of the Uni作者: Malcontent 時(shí)間: 2025-3-30 07:38 作者: Engaged 時(shí)間: 2025-3-30 11:24
Advances in Transplant Dermatology constructed. The standard models contain three essential ingredients: ? The ., which, combined with the observations that the Universe is isotropic, homogeneous and uniformly expanding on a large scale, leads to the Robertson—Walker metric (5.36); ., according to which the world lines of particles 作者: canonical 時(shí)間: 2025-3-30 13:31 作者: 內(nèi)行 時(shí)間: 2025-3-30 16:45 作者: FOLLY 時(shí)間: 2025-3-30 23:29 作者: 售穴 時(shí)間: 2025-3-31 03:04
B. Kadoch,W. J. T. Bos,K. Schneiderer, we examine the case in which it is assumed that all the matter in the Universe, both ‘visible’ and dark, is in baryonic form. This was the natural starting point for the first plausible models for galaxy formation in the 1960s and 1970s, but they are doomed to failure. Despite this, there are tw作者: Albinism 時(shí)間: 2025-3-31 08:09 作者: FLIP 時(shí)間: 2025-3-31 12:40
Worth Your Salt: Halophiles in Education,onting theories of the origin of the large-scale structure of the Universe with observation. The problem addressed in this chapter is how to relate the fluctuations in the dark and baryonic matter on the last scattering surface at the epoch of recombination to the intensity fluctuations which they i
