^ a b c d "model Büyük Patlama."Encyclopædia Britannica. Encyclopædia Britannica Online. Encyclopædia Britannica Inc.^ a b Scientific modelling^ Lemaître, G. (1927). "Un univers homogène de masse constante et de rayon croissant rendant compte de la vitesse radiale des nébuleuses extragalactiques". Annals of the Scientific Society of Brussels 47A: 41. (French) (Translated in: "A Homogeneous Universe of Constant Mass and Growing Radius Accounting for the Radial Velocity of Extragalactic Nebulae". Monthly Notices of the Royal Astronomical Society 91: 483–490. 1931. Expansion of the universe,Lemaître) Lemaître, G. (1931). "The Evolution of the Universe: Discussion". Nature 128: 699–701. doi: 10.1038/128704a0.^ E. Britannica/big-bang-model^ Alpher, R.A.; Bethe, H.; Gamow, G. (1948). "The Origin of Chemical Elements". Physical Review 73: 803. doi: 10.1103/PhysRev.73.803 Gamow^ Hubble, Edwin (1929). "A relation between distance and radial velocity among extra-galactic nebulae". PNAS 15: 168–173.DOI:10.1073/pnas.15.3.168.^ Nucleosynthesis^ BBC News - 'Big bang' astronomer dies^ Foundations of the Big Bang Model,Cosmological principle^ a b c d Isotrope^ Hoyle, F. (1948). "A New Model for the Expanding Universe". Monthly Notices of the Royal Astronomical Society 108: 372. Hoyle^ Friedmann equations^ Penzias, A.A.; Wilson, R.W. (1965). "A Measurement of Excess Antenna Temperature at 4080 Mc/s". Astrophysical Journal 142: 419. doi: 10.1086/148307. Penzias/Wilson^ Elektromanyetik tayfın, gözle görülebilen, dalga boyu 400 nm (mor) ila 750 nm (portakal rengi) arasında değişen kısmı^ Very Large Telescope^ Keck Observatory^ Subaru Telescope^ Raghunathan Srianand, Patrick Petitjean & Cédric Ledoux, The microwave background temperature at the redshift of 2.33771, Nature,408, 931 (2000), astro-ph/0012222 Voir en ligne.^ After 300,000 years, nuclei began to capture electrons and form the first atoms. This cosmic microwave map reveals what the Universe was like after 380,000 years. The red and yellow areas are slightly warmer than the blue and green ones and are a sign that matter was clumping.http://www.infoplease.com/dk/science/encyclopedia/big-bang.html (6) When the cosmic microwave background radiation was emitted during atom formation 300,000 years after the Big Bang, its temperature was several thousand degrees and the light was in the visible part of the electromagnetic spectrum. As the Universe expanded, it cooled and the visible light first became infrared radiation then microwaves. The temperature of the Universe now is a frigid 2.725 degrees about absolute zero. (7) During the period in which atoms were forming and earlier, the Universe was opaque in the sense that light could not travel any appreciable distance. It was as though the Universe was "in a fog." At 380,000 years, recombination was essentially completed: Each proton had paired up with an electron to form a hydrogen atom. Light was liberated. The Universe cleared and the cosmic background radiation has traveled undisturbed ever since. When WMAP makes its measurements, it captures some of the radiation that has been traveling uninterrupted for almost 14 billion years.http://www.jupiterscientific.org/sciinfo/ncupdate.html After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 300,000 years.http://www.wikinfo.org/index.php/Timeline_of_the_Universehttp://map.gsfc.nasa.gov/media/080998/index.html^http://map.gsfc.nasa.gov/media/080998/index.html^ Énergie de masse^ Baryogenesis^ équilibre thermique^ La présence de ces neutrinos influe sur le taux d’expansion de l’univers (voir équations de Friedmann), et par suite sur la vitesse à laquelle l’univers se refroidit, et donc sur la durée de la nucléosynthèse, qui elle-même détermine en partie l’abondance des éléments qui sont synthétisés pendant celle-ci.^ Voir par exemple (İngilizce) Leo Stodolsky, Some neutrino events of the 21st century, in Neutrino astrophysics, comptes rendus du quatrième atelier SFB-375, château de Ringberg, Allemagne, 20-24 octobre 1997, page 178-181, astro-ph/9801320 Voir en ligne.^ Si tel n’était pas le cas, un très fort rayonnement gamma serait émis du voisinage des régions où matière et antimatière coexisteraient. Un tel rayonnement n’est pas observé.^ Kolb and Turner (1988), chapter 6^ Guth, A.H. (1998). The Inflationary Universe: Quest for a New Theory of Cosmic Origins. Vintage Books. ISBN 978-0-09-995950-2.^ a b c Anisotropy^ Fine-tuning^ Courbure spatiale^ Örneğin Planck uzunluğu adıyla bilinen, en küçük uzunluğa yaklaşıldıkça uzay-zamanın tümsek ve çukurlukları artar ve iki nokta arasındaki uzaklık” kavramının hiçbir anlamı kalmaz.^ Flatness problem^ Magnetic monopole^ Bu çözümde "scalar field” terimi yerine, aynı anlamda "inflation" (şişme, şişkinleşme) terimi kullanılmıştır.İlgili bilimsel makaleler^ Scalar field^ Modèle standard^ Weyl curvature hypothesis^ Penrose, R. (1979). "Singularities and Time-Asymmetry". Hawking, S.W. (ed); Israel, W. (ed) General Relativity: An Einstein Centenary Survey: 581–638, Cambridge University Press. Penrose, R. (1989). "Difficulties with Inflationary Cosmology". Fergus, E.J. (ed) Proceedings of the 14th Texas Symposium on Relativistic Astrophysics: 249-264, New York Academy of Sciences. doi: 10.1111/j.1749-6632.1989.tb50513.x., 2^ Spectre de Harrison-Zel'dovich^ Sloan Digital Sky Survey^ Keel, B.. "Dark Matter". Retrieved on 2007-05-28.
