De Sitter universe
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2dF Galaxy Redshift Survey, Age of the universe, Albert Einstein, Alexander Alexandrovich Friedman, Arno Allan Penzias, BOOMERanG experiment, Big Bang, Big Bang nucleosynthesis, COBE, Contributors to Physical cosmology, Cosmic acceleration, Cosmic gravitational wave background, Cosmic inflation, Cosmic microwave background radiation, Cosmic neutrino background, Cosmological constant, Dark Energy Dominated Era, Dark energy, Dark matter, De Sitter space, De Sitter universe, Deceleration parameter, Early universe, Edwin Hubble, Event horizon, Friedmann-Lemaître-Robertson-Walker metric, Friedmann-Robertson-Walker metric, Friedmann equations, Future of an expanding universe, Galaxy, Galaxy filament, Galaxy formation and evolution, General Relativity, George Gamow, George Smoot, Georges Lemaître, Hubble's law, Inflation (cosmology), Isaac Newton, John C. Mather, Lambda-CDM model, Large-scale structure of the cosmos, Local Group, Metric expansion of space, Milky Way, Observational cosmology, Physical cosmology, Planck mass, Planck satellite, Redshift, Reionization, Robert H. Dicke, Robert Woodrow Wilson, Scale factor (Universe), Shape of the Universe, Sloan Digital Sky Survey, Speed of light, Stephen Hawking, Structure formation, Timeline of cosmology, Timeline of the Big Bang, Ultimate fate of the universe, Universe, Vera Rubin, Wilkinson Microwave Anisotropy Probe, Willem de Sitter, Yakov Zel'dovich, A de Sitter universe is a solution to Einstein's field equations of General Relativity which is named after Willem de Sitter. It models the universe as spatially flat and neglects ordinary matter, so the dynamics of the universe are dominated by the cosmological constant, thought to correspond to dark energy.
In astronomy, the 2dF Galaxy Redshift Survey (Two-degree-Field Galaxy Redshift Survey), 2dF or 2dFGRS is a redshift survey conducted by the Anglo-Australian Observatory (AAO) with the 3.9m Anglo-Australian Telescope between 1997 and 11 April 2002.[1] The data from this survey were made public on 30 June 2003. The survey determined the large-scale structure in one section of the local Universe. As of July 2009, it is the second largest redshift survey next to the Sloan Digital Sky Survey which began in 2000. Matthew Colless, Steve Maddox and John Peacock were in charge of the project.
The age of the universe is the time elapsed between the Big Bang and the present day. Current theory and observations suggest that the universe is between 13.5 and 14 billion years old.[1] The uncertainty range has been obtained by the agreement of a number of scientific research projects. These projects included background radiation measurements and more ways to measure the expansion of the universe. Background radiation measurements give the cooling time of the universe since the Big Bang. Expansion of the universe measurements give accurate data to calculate the age of the universe.
Albert Einstein (pronounced /ˈælbərt ˈaɪnstaɪn/; German: [ˈalbɐt ˈaɪ̯nʃtaɪ̯n] (
listen); 14 March 1879–18 April 1955) was a theoretical physicist who is widely regarded as one of the most influential scientists of all time, and the "greatest physicist ever", according to a 1999 poll of leading physicists[3]. His many contributions to physics include the special and general theories of relativity, the founding of relativistic cosmology, the first post-Newtonian expansion, explaining the perihelion advance of Mercury, prediction of the deflection of light by gravity and gravitational lensing, the first fluctuation dissipation theorem which explained the Brownian movement of molecules, the photon theory and wave-particle duality, the quantum theory of atomic motion in solids, the zero-point energy concept, the semiclassical version of the Schrödinger equation, and the quantum theory of a monatomic gas which predicted Bose–Einstein condensation.Alexander Alexandrovich Friedman or Friedmann (Russian: Александр Александрович Фридман) (June 16, 1888, Saint Petersburg, Imperial Russia – September 16, 1925, Leningrad, USSR) was a Russian and Soviet cosmologist and mathematician.
The BOOMERanG experiment (Balloon Observations Of Millimetric Extragalactic Radiation and Geophysics) measured the cosmic microwave background radiation of a part of the sky during three sub-orbital (high altitude) balloon flights. It was the first experiment to make large, high fidelity images of the CMB temperature anisotropies. By using a telescope which flew at over 42,000 meters high, it was possible to reduce the atmospheric absorption of microwaves to a minimum. This allowed massive cost reduction compared to a satellite probe, though only a small part of the sky could be scanned.The Big Bang is the cosmological model of the initial conditions and subsequent development of the Universe that is supported by the most comprehensive and accurate explanations from current scientific evidence and observation.[1][2] As used by cosmologists, the term Big Bang generally refers to the idea that the Universe has expanded from a primordial hot and dense initial condition at some finite time in the past (best available measurements in 2009 suggest that the initial conditions occurred around 13.3 to 13.9 billion years ago[3][4]), and continues to expand to this day.In physical cosmology, Big Bang nucleosynthesis (or primordial nucleosynthesis, abbreviated BBN) refers to the production of nuclei other than those of H-1 (i.e. the normal, light isotope of hydrogen, whose nuclei consist of a single proton each) during the early phases of the universe. Primordial nucleosynthesis took place just a few minutes after the Big Bang and is believed to be responsible for the formation of a heavier isotope of hydrogen known as deuterium (H-2 or D), the helium isotopes He-3 and He-4, and the lithium isotopes Li-6 and Li-7. In addition to these stable nuclei some unstable, or radioactive, isotopes were also produced during primordial nucleosynthesis: tritium or H-3; beryllium-7 (Be-7), and beryllium-8 (Be-8). These unstable isotopes either decayed or fused with other nuclei to make one of the stable isotopes.
The age of the universe is the time elapsed between the Big Bang and the present day. Current theory and observations suggest that the universe is between 13.5 and 14 billion years old.[1] The uncertainty range has been obtained by the agreement of a number of scientific research projects. These projects included background radiation measurements and more ways to measure the expansion of the universe. Background radiation measurements give the cooling time of the universe since the Big Bang. Expansion of the universe measurements give accurate data to calculate the age of the universe.
Albert Einstein (pronounced /ˈælbərt ˈaɪnstaɪn/; German: [ˈalbɐt ˈaɪ̯nʃtaɪ̯n] (
listen); 14 March 1879–18 April 1955) was a theoretical physicist who is widely regarded as one of the most influential scientists of all time, and the "greatest physicist ever", according to a 1999 poll of leading physicists[3]. His many contributions to physics include the special and general theories of relativity, the founding of relativistic cosmology, the first post-Newtonian expansion, explaining the perihelion advance of Mercury, prediction of the deflection of light by gravity and gravitational lensing, the first fluctuation dissipation theorem which explained the Brownian movement of molecules, the photon theory and wave-particle duality, the quantum theory of atomic motion in solids, the zero-point energy concept, the semiclassical version of the Schrödinger equation, and the quantum theory of a monatomic gas which predicted Bose–Einstein condensation.Alexander Alexandrovich Friedman or Friedmann (Russian: Александр Александрович Фридман) (June 16, 1888, Saint Petersburg, Imperial Russia – September 16, 1925, Leningrad, USSR) was a Russian and Soviet cosmologist and mathematician.The BOOMERanG experiment (Balloon Observations Of Millimetric Extragalactic Radiation and Geophysics) measured the cosmic microwave background radiation of a part of the sky during three sub-orbital (high altitude) balloon flights. It was the first experiment to make large, high fidelity images of the CMB temperature anisotropies. By using a telescope which flew at over 42,000 meters high, it was possible to reduce the atmospheric absorption of microwaves to a minimum. This allowed massive cost reduction compared to a satellite probe, though only a small part of the sky could be scanned.The Big Bang is the cosmological model of the initial conditions and subsequent development of the Universe that is supported by the most comprehensive and accurate explanations from current scientific evidence and observation.[1][2] As used by cosmologists, the term Big Bang generally refers to the idea that the Universe has expanded from a primordial hot and dense initial condition at some finite time in the past (best available measurements in 2009 suggest that the initial conditions occurred around 13.3 to 13.9 billion years ago[3][4]), and continues to expand to this day.In physical cosmology, Big Bang nucleosynthesis (or primordial nucleosynthesis, abbreviated BBN) refers to the production of nuclei other than those of H-1 (i.e. the normal, light isotope of hydrogen, whose nuclei consist of a single proton each) during the early phases of the universe. Primordial nucleosynthesis took place just a few minutes after the Big Bang and is believed to be responsible for the formation of a heavier isotope of hydrogen known as deuterium (H-2 or D), the helium isotopes He-3 and He-4, and the lithium isotopes Li-6 and Li-7. In addition to these stable nuclei some unstable, or radioactive, isotopes were also produced during primordial nucleosynthesis: tritium or H-3; beryllium-7 (Be-7), and beryllium-8 (Be-8). These unstable isotopes either decayed or fused with other nuclei to make one of the stable isotopes.