標(biāo)題: Titlebook: Current Topics in Astrofundamental Physics; The Early Universe N. Sánchez,A. Zichichi Book 1995 Springer Science+Business Media Dordrecht 1 [打印本頁] 作者: Capricious 時(shí)間: 2025-3-21 18:45
書目名稱Current Topics in Astrofundamental Physics影響因子(影響力)
書目名稱Current Topics in Astrofundamental Physics影響因子(影響力)學(xué)科排名
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書目名稱Current Topics in Astrofundamental Physics網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Current Topics in Astrofundamental Physics被引頻次
書目名稱Current Topics in Astrofundamental Physics被引頻次學(xué)科排名
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書目名稱Current Topics in Astrofundamental Physics年度引用學(xué)科排名
書目名稱Current Topics in Astrofundamental Physics讀者反饋
書目名稱Current Topics in Astrofundamental Physics讀者反饋學(xué)科排名
作者: GREEN 時(shí)間: 2025-3-21 21:08 作者: 軍火 時(shí)間: 2025-3-22 01:17 作者: 滲入 時(shí)間: 2025-3-22 08:26
Drug Trafficking and Investmentsrtions at longer wavelengths. Is this the end of the story? Can new observations provide significant new understanding of physical processes in the early universe? I review mechanisms which can distort the CMB spectrum and discuss observing strategies to complement the COBE results.作者: 旅行路線 時(shí)間: 2025-3-22 10:18
5G RAN Architecture: C-RAN with NGFI, provide a serious limit to observations. Nevertheless, observations may determine if the evolution of the Universe can be understood from fundamental physical principles. The . Differential Microwave Radiometers (DMR) has mapped the cosmic microwave background anisotropy and measured the primordial density distribution on super-horizon scales.作者: A保存的 時(shí)間: 2025-3-22 15:17
https://doi.org/10.1007/978-3-319-40126-3galaxy clusters. Taken at face value, these two methods give contadictory results, Ω = 1 in the first case, and Ω ≤ 0.5 in the second. These results can be reconciled if, either Ω = 1 and the standard nucleosynthesis constraints are incorrect,or Ω ? 0.4 and galaxies are substantially less clustered than the dark mass.作者: A保存的 時(shí)間: 2025-3-22 19:43
1389-2185 cture formation, and the interplay between them. Theemphasis is on the mutual impact of fundamental physics and cosmology,both at theoretical and experimental (observational) levels within adeep, well- focused and well-defined programme. .The nature of the domain itself leads to different aspects, a作者: Stress-Fracture 時(shí)間: 2025-3-22 23:02
Joanna Zyla,Michal Marczyk,Joanna Polanskar scale..A review of observational results on scales ranging from arcseconds to arcminutes, with an emphasis on interferometric measurements at the Very Large Array. The Sunyaev-Zel’dovich effect is treated as both a signal and a source of foreground “noise.”作者: Watemelon 時(shí)間: 2025-3-23 01:49 作者: intellect 時(shí)間: 2025-3-23 09:00
A. Vinod Yeldho Baby,B. Rajesh G. the last scattering of relict radiation. These anomalies are the consequences of Sakharov oscillations and we call them Long Distance Correlations (LDCs). We investigate the dependence of the properties of the LDCs from the parameters of the models and emphasize that the properties are very sensitive to the nature of dark matter.作者: intoxicate 時(shí)間: 2025-3-23 11:43 作者: Noisome 時(shí)間: 2025-3-23 17:11 作者: 高射炮 時(shí)間: 2025-3-23 19:27
New Multicarrier Modulations for 5G angular scales against the hypothesis that the observed temperature fluctuations reflect Gaussian initial density perturbations with random phases. The data are in excellent agreement with the Gaussian hypothesis and rule out certain “toy models” of non-Gaussian amplitude distribution.作者: 擁擠前 時(shí)間: 2025-3-23 23:02
Izzat Darwazeh,Ryan C. Grammenos,Tongyang Xun conjunction with X-ray maps from the ROSAT and Einstein satellites to place a limit on the Hubble constant of.. The implications of these observations are discussed in the context of continued CMB observations from ground-based sites and plans are presented for the Very Small Array.作者: 群居動(dòng)物 時(shí)間: 2025-3-24 05:51
A.E. Lutsky,I.V. Mursenkova,I.A. Znamenskayanal error). Eight methods that are independent of the Virgo cluster (Table 3) give H. = 50 within 10%. Criticisms of all the methods that have been said to give the short distance scale with H. ~ 85 are set out.作者: excrete 時(shí)間: 2025-3-24 09:20 作者: 前兆 時(shí)間: 2025-3-24 12:13 作者: aqueduct 時(shí)間: 2025-3-24 15:28 作者: 注意力集中 時(shí)間: 2025-3-24 19:32 作者: Ancillary 時(shí)間: 2025-3-25 01:58
The Covariant and Gauge Invariant Approach to Perturbations in Cosmologyhe best available approach to proving spatial homogeneity of the universe. The extension of this approach to Sachs-Wolfe style analyses is not yet complete, and a series of issues to do with averaging scales and with modelling the real, lumpy universe by means of simpler, smoothed out models remain to be resolved.作者: 輕打 時(shí)間: 2025-3-25 03:37 作者: 行為 時(shí)間: 2025-3-25 10:11 作者: 被詛咒的人 時(shí)間: 2025-3-25 12:01 作者: 整頓 時(shí)間: 2025-3-25 19:39
Dark Matter and the Value of Ωgalaxy clusters. Taken at face value, these two methods give contadictory results, Ω = 1 in the first case, and Ω ≤ 0.5 in the second. These results can be reconciled if, either Ω = 1 and the standard nucleosynthesis constraints are incorrect,or Ω ? 0.4 and galaxies are substantially less clustered than the dark mass.作者: 機(jī)構(gòu) 時(shí)間: 2025-3-25 23:36 作者: Pudendal-Nerve 時(shí)間: 2025-3-26 01:55
Lectures on Inflationary Cosmologyty and temperature. With the rapid expansion of the Universe the average energy of particles, given by the temperature, decreased rapidly, and the Universe became cold. This theory became especially popular after the discovery of the microwave background radiation. However, by the end of the 70’s it作者: BRIEF 時(shí)間: 2025-3-26 05:50
Back Reaction of Strings in Self Consistent String Cosmologyd D-dimensional universes are treated for any expansion factor R. Strings obey the perfect fluid relation p = (γ - 1)p with three different behaviours: (i) Unstable for R → ∞ with growing energy density ρ ~ R., . pressure, and γ = (D - 2)/(D - 1) for inflationary universes; (ii) Dual for R → 0, with作者: 賞心悅目 時(shí)間: 2025-3-26 10:01
Cosmological Inflation, Microwave Background Anisotropies and Large Scale Structure of the Universe-Jacobi methods, I will describe . how to compute density fluctuations and cosmic microwave anisotropies arising from inflation, and . improvements of the Zel’dovich approximation describing gravitational collapse. I compare these results with the latest cosmological observations.作者: 發(fā)電機(jī) 時(shí)間: 2025-3-26 15:21 作者: FEIGN 時(shí)間: 2025-3-26 19:06
The Big Bang and the Infrared Sky as Seen by Cobehe early universe. It also measured emission from nearby sources such as the stars, dust, molecules, atoms, ions, and electrons in the Milky Way, and dust and comets in the Solar System. It was launched 18 November 1989 on a Delta rocket, carrying one microwave instrument and two cryogenically coole作者: Psa617 時(shí)間: 2025-3-26 21:35 作者: 考博 時(shí)間: 2025-3-27 05:00 作者: Narcissist 時(shí)間: 2025-3-27 08:51
Cosmic Microwave Background Anisotropy Large Angular Scales / Cobe DMR Resultssts of various ideas of large scale structure formation. CMB observations now let us test the role of gravity and General Relativity in cosmology including the geometry, topology, and dynamics of the Universe. Foreground galactic emissions, dust thermal emission and emission from energetic electrons作者: 軍火 時(shí)間: 2025-3-27 11:45 作者: novelty 時(shí)間: 2025-3-27 16:47
Detections of Primary and Secondary Anisotropies in the CMBthe three CMB programmes currently underway at MRAO Cambridge. Results are presented from the Tenerife experiments observing on ~ 5° scales at frequencies of 10, 15 and 33 GHz. The best scan attains a sensitivity ~20μK and clear features are present with the properties expected for CMB anisotropy. O作者: 金盤是高原 時(shí)間: 2025-3-27 19:23 作者: arthroscopy 時(shí)間: 2025-3-27 22:48 作者: Ballerina 時(shí)間: 2025-3-28 05:33 作者: Abduct 時(shí)間: 2025-3-28 09:50 作者: entrance 時(shí)間: 2025-3-28 12:03 作者: 難解 時(shí)間: 2025-3-28 17:39
1389-2185 ous view of the field. ..Audience:. experimentalists and theoreticians from a variety ofbackgrounds: physics, astrophysics and astronomy. An excellentreference for post-doctoral scientists. Useful for senior scientistsand advanced graduate students. .978-94-010-4046-4978-94-011-0095-3Series ISSN 1389-2185 作者: 妨礙 時(shí)間: 2025-3-28 18:57 作者: 羞辱 時(shí)間: 2025-3-29 02:36 作者: 暴發(fā)戶 時(shí)間: 2025-3-29 06:51 作者: POINT 時(shí)間: 2025-3-29 09:07
The Big Bang and the Infrared Sky as Seen by Cobe differs from a blackbody by less than 0.03%. The Diffuse Infrared Background Experiment (DIRBE) spanned the wavelength range from 1.2 to 240 inn and mapped the sky at a wide range of solar elongation angles to distinguish foreground sources from a possible extragalactic Cosmic Infrared Background R作者: apiary 時(shí)間: 2025-3-29 13:52 作者: 潛移默化 時(shí)間: 2025-3-29 18:06
https://doi.org/10.1007/978-3-319-20046-0variant approach in which the variables used have a transparent physical and geometric meaning. A kinetic-theory version of this approach can be used to study anisotropies in the Cosmic Background Radiation (CBR), and in particular to generalise the Ehlers-Geren-Sachs theorem which is the basis of t作者: 序曲 時(shí)間: 2025-3-29 22:00 作者: Paleontology 時(shí)間: 2025-3-30 01:27
Ulrich Spandau,Mitrofanis Pavlidisd D-dimensional universes are treated for any expansion factor R. Strings obey the perfect fluid relation p = (γ - 1)p with three different behaviours: (i) Unstable for R → ∞ with growing energy density ρ ~ R., . pressure, and γ = (D - 2)/(D - 1) for inflationary universes; (ii) Dual for R → 0, with作者: TAIN 時(shí)間: 2025-3-30 05:44 作者: FADE 時(shí)間: 2025-3-30 08:24
Important Vitreoretinal Techniques with 27Ganisotropy in the cosmic microwave background radiation is caused by the long-wavelength cosmological perturbations of quantum mechanical origin, they are, most likely, gravitational waves, rather than density perturbations or rotational perturbations. Some disagreements with previous publications a作者: 整體 時(shí)間: 2025-3-30 16:24
Niels Neumann,Ronny Henker,Marcus S. Dahlemhe early universe. It also measured emission from nearby sources such as the stars, dust, molecules, atoms, ions, and electrons in the Milky Way, and dust and comets in the Solar System. It was launched 18 November 1989 on a Delta rocket, carrying one microwave instrument and two cryogenically coole作者: 收集 時(shí)間: 2025-3-30 19:36 作者: keloid 時(shí)間: 2025-3-30 21:50
https://doi.org/10.1007/978-3-319-32585-9e-scale structure forms as the result of gravitational amplification of initially small perturbations in the primordial density distribution. These density perturbations leave their imprint as anisotropies in the Cosmic Microwave Background (CMB) radiation. The . Differential Microwave Radiometers (作者: gastritis 時(shí)間: 2025-3-31 01:39
5G RAN Architecture: C-RAN with NGFIsts of various ideas of large scale structure formation. CMB observations now let us test the role of gravity and General Relativity in cosmology including the geometry, topology, and dynamics of the Universe. Foreground galactic emissions, dust thermal emission and emission from energetic electrons作者: 蝕刻 時(shí)間: 2025-3-31 05:42 作者: BUMP 時(shí)間: 2025-3-31 12:58 作者: 連接 時(shí)間: 2025-3-31 15:42
Joanna Zyla,Michal Marczyk,Joanna Polanskanal techniques used in different ranges of angular scale to detect them. A review of sources of foreground noise that dominate in each range of angular scale..A review of observational results on scales ranging from arcseconds to arcminutes, with an emphasis on interferometric measurements at the Ve
