標(biāo)題: Titlebook: Dynamical Systems and Cosmology; A. A. Coley Book 2003 Springer Science+Business Media Dordrecht 2003 Cosmology.EFE.Gravity.Potential.Rela [打印本頁(yè)] 作者: 無(wú)限 時(shí)間: 2025-3-21 18:00
書(shū)目名稱(chēng)Dynamical Systems and Cosmology影響因子(影響力)
書(shū)目名稱(chēng)Dynamical Systems and Cosmology影響因子(影響力)學(xué)科排名
書(shū)目名稱(chēng)Dynamical Systems and Cosmology網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱(chēng)Dynamical Systems and Cosmology網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱(chēng)Dynamical Systems and Cosmology被引頻次
書(shū)目名稱(chēng)Dynamical Systems and Cosmology被引頻次學(xué)科排名
書(shū)目名稱(chēng)Dynamical Systems and Cosmology年度引用
書(shū)目名稱(chēng)Dynamical Systems and Cosmology年度引用學(xué)科排名
書(shū)目名稱(chēng)Dynamical Systems and Cosmology讀者反饋
書(shū)目名稱(chēng)Dynamical Systems and Cosmology讀者反饋學(xué)科排名
作者: Proclaim 時(shí)間: 2025-3-21 20:28
Trendüberwachung über Lebensdauersional. On the other hand, .—theory, defined originally in terms of the strongly coupled limit of the type IIA superstring, is an eleven—dimensional theory. It is widely believed that eleven—dimensional supergravity represents the low—energy limit of .—theory [337, 376].作者: Antagonist 時(shí)間: 2025-3-22 03:05
String Cosmology,sional. On the other hand, .—theory, defined originally in terms of the strongly coupled limit of the type IIA superstring, is an eleven—dimensional theory. It is widely believed that eleven—dimensional supergravity represents the low—energy limit of .—theory [337, 376].作者: kidney 時(shí)間: 2025-3-22 08:32 作者: mydriatic 時(shí)間: 2025-3-22 10:59 作者: 做事過(guò)頭 時(shí)間: 2025-3-22 12:52
978-90-481-6329-8Springer Science+Business Media Dordrecht 2003作者: 做事過(guò)頭 時(shí)間: 2025-3-22 18:42
Covid-19 sch?rft den Blick für WerteWe shall begin by presenting a brief review of the qualitative theory of ODE [169, 181, 182, 373] , with particular emphasis on those aspects of the non-linear theory of importance in cosmology.作者: exquisite 時(shí)間: 2025-3-23 01:13
https://doi.org/10.1007/978-3-662-62542-2Let us discuss some of the more physically important results of the last Chapter in more detail.作者: 抵消 時(shí)間: 2025-3-23 03:09 作者: 圣人 時(shí)間: 2025-3-23 07:50 作者: Explosive 時(shí)間: 2025-3-23 11:51 作者: 致詞 時(shí)間: 2025-3-23 17:31 作者: 卷發(fā) 時(shí)間: 2025-3-23 22:00
https://doi.org/10.1007/978-3-662-62542-2nd Coley [91] and references therein). Exact spatially homogeneous solutions were first displayed in early papers [135]; however, it was not until after 1985 that many of them were recognized by Wainwright [358] and Rosquist and Jantzen [202, 309] as being selfsimilar. The complete set of self-simil作者: 松果 時(shí)間: 2025-3-23 23:17
,Einführung in die werteorientierte Führung,-interacting scalar field with an exponential potential in the class of Bianchi type B models (except for the exceptional case Bianchi VI.), using the Hewitt and Wainwright formalism [178, 363] . In particular, we shall study the generality of the scaling solutions. We define the governing equations作者: GEON 時(shí)間: 2025-3-24 03:14 作者: 臨時(shí)抱佛腳 時(shí)間: 2025-3-24 06:30 作者: 的闡明 時(shí)間: 2025-3-24 14:26 作者: 減少 時(shí)間: 2025-3-24 15:31 作者: arbovirus 時(shí)間: 2025-3-24 20:57 作者: 擔(dān)心 時(shí)間: 2025-3-25 00:21
Trendüberwachung über Lebensdauer determine (among other things) whether models evolve from a low-curvature regime and thereby test the self-consistency of the low-energy effective string cosmology paradigm. In particular, we consider the class of “isotropic curvature” models [265, 314] , which are spatially homogeneous but contain作者: 高原 時(shí)間: 2025-3-25 03:55
Trendüberwachung über Lebensdaueroduli space of a more fundamental, non-perturbative theory known as M-theory [376], and so no particular string theory is necessarily more fundamental since they are all related by duality symmetries (for a review see, e.g., Ref. [321]). Moreover, another point of this moduli space corresponds to el作者: 繼而發(fā)生 時(shí)間: 2025-3-25 11:32 作者: 保全 時(shí)間: 2025-3-25 12:37
,Einführung in die werteorientierte Führung, differential equations (ODE). Inhomogeneous cosmological models can also be studied, but since the evolution equations are autonomous partial differential equations (PDE) in this case the resulting state space is infinite-dimensional (i.e., a function space) , and the analysis is considerably more complicated.作者: 大溝 時(shí)間: 2025-3-25 18:17
Mehr Dinge zwischen Himmel und Erderedict steep exponential potentials [164] (i.e., .. > 2), effectively eliminating the possibility of power-law inflation. However, dimensionally reduced higher-dimensional theories also predict numerous scalar fields, and so it is of interest to study models with multiple scalar fields.作者: forecast 時(shí)間: 2025-3-25 20:17
Introduction, differential equations (ODE). Inhomogeneous cosmological models can also be studied, but since the evolution equations are autonomous partial differential equations (PDE) in this case the resulting state space is infinite-dimensional (i.e., a function space) , and the analysis is considerably more complicated.作者: 引導(dǎo) 時(shí)間: 2025-3-26 03:59
Multiple Scalar Fields,redict steep exponential potentials [164] (i.e., .. > 2), effectively eliminating the possibility of power-law inflation. However, dimensionally reduced higher-dimensional theories also predict numerous scalar fields, and so it is of interest to study models with multiple scalar fields.作者: 口味 時(shí)間: 2025-3-26 06:58
Scalar Tensor Theories of Gravity,] and Brans and Dicke [60] and the most general scalar-tensor theories were formulated by Bergmann [40], Nordtvedt [289] and Wagoner [356] . The observational limits on scalar-tensor theories include solar system tests [2, 59, 64, 189] and cosmological tests such as Big Bang nucleosynthesis constraints [17, 322].作者: OATH 時(shí)間: 2025-3-26 11:00
M-Theory, since they are all related by duality symmetries (for a review see, e.g., Ref. [321]). Moreover, another point of this moduli space corresponds to eleven-dimensional supergravity. This represents the low-energy limit of M-theory [337, 376] .作者: judiciousness 時(shí)間: 2025-3-26 14:26 作者: 雜色 時(shí)間: 2025-3-26 18:14 作者: 桉樹(shù) 時(shí)間: 2025-3-27 00:50
Trendüberwachung über Lebensdauer non-trivial curvature and anisotropy and are characterized by the fact that the 3-dimensional Ricci curvature tensor is isotropic; i.e., .. is proportional to .. on the spatial hypersurfaces and these surfaces therefore have constant curvature . [265].作者: optional 時(shí)間: 2025-3-27 05:00 作者: 自傳 時(shí)間: 2025-3-27 07:02
Scalar Field Cosmologies with Barotropic Matter,, which are modified from those developed in [363], and discuss the invariant sets and the existence of monotonic functions. We then classify and list all of the equilibrium points, and their local stability is discussed. We present a detailed analysis and conclude with a discussion.作者: 有權(quán)威 時(shí)間: 2025-3-27 12:17 作者: MIME 時(shí)間: 2025-3-27 16:29 作者: 攤位 時(shí)間: 2025-3-27 20:24
0067-0057 ical models, particularly when the governing equations are a finite system of autonomous ordinary differential equations. .In this book we discuss cosmological models as dynamical systems, with particular emphasis on applications in the early Universe. We point out the important role of self-similar作者: 冒煙 時(shí)間: 2025-3-28 00:17 作者: 過(guò)份好問(wèn) 時(shí)間: 2025-3-28 04:10 作者: 草率女 時(shí)間: 2025-3-28 07:10 作者: 清楚 時(shí)間: 2025-3-28 11:07
Der seltsame Kollaps von Kopenhagen reasons could be the perceived weakness of the field effects or the lack, as yet, of a consistent theory explaining the origin of cosmic magnetism. However, this situation has changed considerably recently (cf. [161]).作者: shrill 時(shí)間: 2025-3-28 18:37
Closed Models,lysis. In this Chapter we shall discuss the qualitative properties of the positive-curvature FRW models and the Kantowski-Sachs models with a barotropic fluid and a non-interacting scalar field with an exponential potential [96].作者: 小隔間 時(shí)間: 2025-3-28 21:33 作者: 巫婆 時(shí)間: 2025-3-28 23:31
Introduction,al cosmology involves the study of the early- and late- time behaviour of more general classes of cosmological models as well as the detailed investigation of special exact cosmological solutions with symmetries such as the spatially homogeneous and isotropic models with a Robertson-Walker (RW) geom作者: 慢跑 時(shí)間: 2025-3-29 04:41 作者: 津貼 時(shí)間: 2025-3-29 09:50 作者: Seminar 時(shí)間: 2025-3-29 12:58 作者: Entirety 時(shí)間: 2025-3-29 15:46
Multiple Scalar Fields,7] . There are a variety of inflationary models which include scalar fields [291], and in scalar field models with an exponential potential [372] the universe inflates at a power-law rate, .(.) ∞ .., where . > 1 [249]. As we have seen, all ever-expanding scalar field models with an exponential poten作者: defibrillator 時(shí)間: 2025-3-29 21:59
Scalar Tensor Theories of Gravity,string theory (see [188] and references therein) . The first scalar-tensor theories to appear (with . = .. ) were due to Jordan [205, 206], Fierz [146] and Brans and Dicke [60] and the most general scalar-tensor theories were formulated by Bergmann [40], Nordtvedt [289] and Wagoner [356] . The obser作者: osteocytes 時(shí)間: 2025-3-30 03:19 作者: set598 時(shí)間: 2025-3-30 05:22 作者: ELUC 時(shí)間: 2025-3-30 09:56
Anisotropic and Curved String Cosmologies, determine (among other things) whether models evolve from a low-curvature regime and thereby test the self-consistency of the low-energy effective string cosmology paradigm. In particular, we consider the class of “isotropic curvature” models [265, 314] , which are spatially homogeneous but contain作者: Protein 時(shí)間: 2025-3-30 14:29
M-Theory,oduli space of a more fundamental, non-perturbative theory known as M-theory [376], and so no particular string theory is necessarily more fundamental since they are all related by duality symmetries (for a review see, e.g., Ref. [321]). Moreover, another point of this moduli space corresponds to el作者: MOT 時(shí)間: 2025-3-30 18:28
