The Big Bang Theory: The Complete Series [DVD] [2007]

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Cuoco Sweeting: People always ask if we eat the food (during scenes). I must be the only one who really eats the food. I save my appetite until we do those scenes – I want to look real, man! In the mid-1990s, observations of certain globular clusters appeared to indicate that they were about 15billion years old, which conflicted with most then-current estimates of the age of the universe (and indeed with the age measured today). This issue was later resolved when new computer simulations, which included the effects of mass loss due to stellar winds, indicated a much younger age for globular clusters. [80] Hubble's law implies that the universe is uniformly expanding everywhere. This cosmic expansion was predicted from general relativity by Friedmann in 1922 [58] and Lemaître in 1927, [61] well before Hubble made his 1929 analysis and observations, and it remains the cornerstone of the Big Bang model as developed by Friedmann, Lemaître, Robertson, and Walker. Negative pressure is believed to be a property of vacuum energy, but the exact nature and existence of dark energy remains one of the great mysteries of the Big Bang. Results from the WMAP team in 2008 are in accordance with a universe that consists of 73% dark energy, 23% dark matter, 4.6% regular matter and less than 1% neutrinos. [38] According to theory, the energy density in matter decreases with the expansion of the universe, but the dark energy density remains constant (or nearly so) as the universe expands. Therefore, matter made up a larger fraction of the total energy of the universe in the past than it does today, but its fractional contribution will fall in the far future as dark energy becomes even more dominant. [ citation needed] So, if you wait long enough, eventually, a distant galaxy will reach the speed of light. What that means is that even light won't be able to bridge the gap that's being opened between that galaxy and us. There's no way for extraterrestrials on that galaxy to communicate with us, to send any signals that will reach us, once their galaxy is moving faster than light relative to us."

Big Bang Theory (Seasons 1-5) - 16-DVD Box Set ( The Big The Big Bang Theory (Seasons 1-5) - 16-DVD Box Set ( The Big

Using Big Bang models, it is possible to calculate the expected concentration of the isotopes helium-4 ( 4He), helium-3 ( 3He), deuterium ( 2H), and lithium-7 ( 7Li) in the universe as ratios to the amount of ordinary hydrogen. [34] The relative abundances depend on a single parameter, the ratio of photons to baryons. This value can be calculated independently from the detailed structure of CMB fluctuations. The ratios predicted (by mass, not by abundance) are about 0.25 for 4He:H, about 10 −3 for 2H:H, about 10 −4 for 3He:H, and about 10 −9 for 7Li:H. [34] Thursday Finals: 'Big Bang Theory,' 'The X Factor,' 'Parks & Recreation' and 'Whitney' Adjusted Up|publisher=TV by the Numbers Over a long period of time, the slightly denser regions of the uniformly distributed matter gravitationally attracted nearby matter and thus grew even denser, forming gas clouds, stars, galaxies, and the other astronomical structures observable today. [1] The details of this process depend on the amount and type of matter in the universe. The four possible types of matter are known as cold dark matter (CDM), warm dark matter, hot dark matter, and baryonic matter. The best measurements available, from the Wilkinson Microwave Anisotropy Probe (WMAP), show that the data is well-fit by a Lambda-CDM model in which dark matter is assumed to be cold. (Warm dark matter is ruled out by early reionization.) [37] This CDM is estimated to make up about 23% of the matter/energy of the universe, while baryonic matter makes up about 4.6%. [38] During the 1970s and the 1980s, various observations showed that there is not sufficient visible matter in the universe to account for the apparent strength of gravitational forces within and between galaxies. This led to the idea that up to 90% of the matter in the universe is dark matter that does not emit light or interact with normal baryonic matter. In addition, the assumption that the universe is mostly normal matter led to predictions that were strongly inconsistent with observations. In particular, the universe today is far more lumpy and contains far less deuterium than can be accounted for without dark matter. While dark matter has always been controversial, it is inferred by various observations: the anisotropies in the CMB, galaxy cluster velocity dispersions, large-scale structure distributions, gravitational lensing studies, and X-ray measurements of galaxy clusters. [128] Hawley, John F.; Holcomb, Katherine A. (7 July 2005). Foundations of Modern Cosmology. OUP Oxford. p.355. ISBN 9780198530961.

The magnetic monopole objection was raised in the late 1970s. Grand unified theories (GUTs) predicted topological defects in space that would manifest as magnetic monopoles. These objects would be produced efficiently in the hot early universe, resulting in a density much higher than is consistent with observations, given that no monopoles have been found. This problem is resolved by cosmic inflation, which removes all point defects from the observable universe, in the same way that it drives the geometry to flatness. [131] Flatness problem The overall geometry of the universe is determined by whether the Omega cosmological parameter is less than, equal to or greater than 1. Shown from top to bottom are a closed universe with positive curvature, a hyperbolic universe with negative curvature and a flat universe with zero curvature. Hoyle, Fred (October 1948). "A New Model for the Expanding Universe". Monthly Notices of the Royal Astronomical Society. 108 (5): 372–382. Bibcode: 1948MNRAS.108..372H. doi: 10.1093/mnras/108.5.372. The Big Bang explains the evolution of the universe from a starting density and temperature that is well beyond humanity's capability to replicate, so extrapolations to the most extreme conditions and earliest times are necessarily more speculative. Lemaître called this initial state the " primeval atom" while Gamow called the material " ylem". How the initial state of the universe originated is still an open question, but the Big Bang model does constrain some of its characteristics. For example, specific laws of nature most likely came to existence in a random way, but as inflation models show, some combinations of these are far more probable. [140] A flat universe implies a balance between gravitational potential energy and other energy forms, requiring no additional energy to be created. [133] [134] We will see distant galaxies moving away from us, but their speed is increasing with time," Harvard University astronomer Avi Loeb said in a March 2014 Space.com article.

The Big Bang Theory: The Complete Series [Blu-ray] [2007

The Big Bang models developed from observations of the structure of the universe and from theoretical considerations. In 1912, Vesto Slipher measured the first Doppler shift of a " spiral nebula" (spiral nebula is the obsolete term for spiral galaxies), and soon discovered that almost all such nebulae were receding from Earth. He did not grasp the cosmological implications of this fact, and indeed at the time it was highly controversial whether or not these nebulae were "island universes" outside our Milky Way. [56] [57] Ten years later, Alexander Friedmann, a Russian cosmologist and mathematician, derived the Friedmann equations from the Einstein field equations, showing that the universe might be expanding in contrast to the static universe model advocated by Albert Einstein at that time. [58] The universe is not only expanding, but expanding faster. This means that with time, nobody will be able to spot other galaxies from Earth or any other vantage point within our galaxy. Translated in: Lemaître, Georges (March 1931). "A Homogeneous Universe of Constant Mass and Increasing Radius accounting for the Radial Velocity of Extra-galactic Nebulæ". Monthly Notices of the Royal Astronomical Society. 91 (5): 483–490. Bibcode: 1931MNRAS..91..483L. doi: 10.1093/mnras/91.5.483. Heisenberg's uncertainty principle predicts that during the inflationary phase there would be quantum thermal fluctuations, which would be magnified to a cosmic scale. These fluctuations served as the seeds for all the current structures in the universe. [102] :207 Inflation predicts that the primordial fluctuations are nearly scale invariant and Gaussian, which has been confirmed by measurements of the CMB. [82] :sec 6 Eddington, Arthur S. (21 March 1931). "The End of the World: from the Standpoint of Mathematical Physics". Nature. 127 (3203): 447–453. Bibcode: 1931Natur.127..447E. doi: 10.1038/127447a0. S2CID 4140648.

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Melchiorri, Alessandro; Ade, Peter A.R.; de Bernardis, Paolo; etal. (20 June 2000). "A Measurement of Ω from the North American Test Flight of Boomerang". The Astrophysical Journal Letters. 536 (2): L63–L66. arXiv: astro-ph/9911445. Bibcode: 2000ApJ...536L..63M. doi: 10.1086/312744. PMID 10859119. S2CID 27518923. Dark energy in its simplest formulation is modeled by a cosmological constant term in Einstein field equations of general relativity, but its composition and mechanism are unknown. More generally, the details of its equation of state and relationship with the Standard Model of particle physics continue to be investigated both through observation and theory. [9]