Ordinary matter, which can lose energy by radiation, forms dense objects and also gas clouds when it collapses. In order to get a, universe (which was the accepted viewn 1917 when the theory was first published), he introduced a “fudge factor”, the “cosmological constant”, to cancel out the effects of gravity. It is somewhat misleading, however, to describe the expansion as some type of explosion of matter away from some particular point in space. Big Crunch will produce a new Big Bang and the process Moreover, we are designed to be curious.

(No observation we have made allows us to look back beyond the moment at which the expansion began.) In this kind of extreme timescale, extremely rare quantum phenomena may also occur that are extremely unlikely to be seen on a timescale smaller than trillions of years. Between about 2 and 20 minutes after the Big Bang, the temperature and pressure of the universe allowed nuclear fusion to occur, giving rise to nuclei of a few light elements beyond hydrogen ("Big Bang nucleosynthesis"). *Your comment will be reviewed before being published. The chronology of the universe describes the history and future of the universe according to Big Bang cosmology. From about 9.8 billion years of cosmic time,[7] the universe's large-scale behaviour is believed to have gradually changed for the third time in its history. First we should remember that, in keeping with what we have already said, more than three quarters of our Cosmos is now a form of that mysterious entity we call dark energy, and more than 85% of the rest is what is called “dark matter,” which we cannot see because, though it interacts with gravity, it does not interact with radiation. Much has been written about time’s arrow, trying to discover where the evolution of our Universe is headed and, since it had a beginning, finding out what its end will be. If supersymmetry is a property of our universe, then it must be broken at an energy that is no lower than 1 TeV, the electroweak scale. The Standard Model of cosmology attempts to explain how the universe physically developed once that moment happened. Gravitational attraction also gradually pulls galaxies towards each other to form groups, clusters and superclusters. Even though such a region is subject to overall expansion, the excess of matter leads it to contract, creating a linked object, which may be a star, a stellar cumulus, or a galaxy. Advances in particle physics suggest some interesting ways these questions might be answered; the challenge is to find experimental tests of the ideas. In the case of indefinitely continuing metric expansion of space, the energy density in the universe will decrease until, after an estimated time of 10, Expansion of space accelerates and at some point becomes so extreme that even subatomic particles and the fabric of, For any value of the dark energy content of the universe where the negative pressure ratio is less than -1, the expansion rate of the universe will continue to increase without limit. (or is it just me...), Smithsonian Privacy However, the intersection point ρmat. They can be huge as well as perhaps small—and non-metallic (no elements except hydrogen and helium). This was the period in the evolution of the early universe immediately after electroweak symmetry breaking, when the fundamental interactions of gravitation, electromagnetism, the strong interaction and the weak interaction had taken their present forms, but the temperature of the universe was still too high to allow quarks to bind together to form hadrons. The singularity from the FLRW metric is interpreted to mean that current theories are inadequate to describe what actually happened at the start of the Big Bang itself.

By far the most accepted understanding is that this is due to an unknown form of energy which has been given the name "dark energy". In contrast, the redshift of very distant objects—radio galaxies and quasars—is an awesome phenomenon; some appear to be moving away at greater than 90 percent of the speed of light.

Thus, to imagine a Universe that is mechanically regulated like some sort of perfect clock is the farthest thing from reality. On a large scale, the Universe we can now contemplate with our telescopes appears to be a little more that 13,000 million years old, and enormously empty. The earliest structures to form are the first stars (known as Population III stars), dwarf galaxies, and quasars (which are thought to be bright, early active galaxies containing a supermassive black hole surrounded by an inward-spiralling accretion disk of gas). (In other words, that there was a beginning to the universe.) Those models do not even call for more than three dimensions, despite the fact that some theories, such as “string theory,” call for a few more. A galaxy emits or absorbs some wavelengths of light more strongly than others. Therefore, in inflationary cosmology, the earliest meaningful time "after the Big Bang" is the time of the end of inflation.

[35][36], The amounts of each light element in the early universe can be estimated from old galaxies, and is strong evidence for the Big Bang. According to traditional Big Bang cosmology, the electroweak epoch began 10−36 seconds after the Big Bang, when the temperature of the universe was low enough (1028 K) for the electronuclear force to begin to manifest as two separate interactions, the strong and the electroweak interactions. This indicates that, in finding the intersection, one should not neglect the curvature term in the general equation of the expanding universe.

Which of them will happen, if any, depends on the precise values of physical constants such as the cosmological constant, the possibility of proton decay, the energy of the vacuum (meaning, the energy of "empty" space itself), and the natural laws beyond the Standard Model. These clumps, which had seeds in the fluctuations in the CMB spectrum (shown in Figure 3), were denser than their surroundings by only about one part in 100,000.

When they compared the data they obtained with those galaxies’ red shift—which measures the expansion of the Universe—they were surprised to discover that, the further away the galaxies, the slower the rate of expansion. [66] More recent observations have shown these ages to be shorter than previously indicated. Today, the Universe continues to expand. /

[63] (This age estimate is now believed to be slightly overstated).[64]. Based upon the emerging science of nucleocosmochronology, the Galactic thin disk of the Milky Way is estimated to have been formed 8.8 ± 1.7 billion years ago.[6]. This article was originally published with the title "The Evolution of the Universe" in Scientific American 271, 4, 52-57 (October 1994).

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Ordinary matter, which can lose energy by radiation, forms dense objects and also gas clouds when it collapses. In order to get a, universe (which was the accepted viewn 1917 when the theory was first published), he introduced a “fudge factor”, the “cosmological constant”, to cancel out the effects of gravity. It is somewhat misleading, however, to describe the expansion as some type of explosion of matter away from some particular point in space. Big Crunch will produce a new Big Bang and the process Moreover, we are designed to be curious.

(No observation we have made allows us to look back beyond the moment at which the expansion began.) In this kind of extreme timescale, extremely rare quantum phenomena may also occur that are extremely unlikely to be seen on a timescale smaller than trillions of years. Between about 2 and 20 minutes after the Big Bang, the temperature and pressure of the universe allowed nuclear fusion to occur, giving rise to nuclei of a few light elements beyond hydrogen ("Big Bang nucleosynthesis"). *Your comment will be reviewed before being published. The chronology of the universe describes the history and future of the universe according to Big Bang cosmology. From about 9.8 billion years of cosmic time,[7] the universe's large-scale behaviour is believed to have gradually changed for the third time in its history. First we should remember that, in keeping with what we have already said, more than three quarters of our Cosmos is now a form of that mysterious entity we call dark energy, and more than 85% of the rest is what is called “dark matter,” which we cannot see because, though it interacts with gravity, it does not interact with radiation. Much has been written about time’s arrow, trying to discover where the evolution of our Universe is headed and, since it had a beginning, finding out what its end will be. If supersymmetry is a property of our universe, then it must be broken at an energy that is no lower than 1 TeV, the electroweak scale. The Standard Model of cosmology attempts to explain how the universe physically developed once that moment happened. Gravitational attraction also gradually pulls galaxies towards each other to form groups, clusters and superclusters. Even though such a region is subject to overall expansion, the excess of matter leads it to contract, creating a linked object, which may be a star, a stellar cumulus, or a galaxy. Advances in particle physics suggest some interesting ways these questions might be answered; the challenge is to find experimental tests of the ideas. In the case of indefinitely continuing metric expansion of space, the energy density in the universe will decrease until, after an estimated time of 10, Expansion of space accelerates and at some point becomes so extreme that even subatomic particles and the fabric of, For any value of the dark energy content of the universe where the negative pressure ratio is less than -1, the expansion rate of the universe will continue to increase without limit. (or is it just me...), Smithsonian Privacy However, the intersection point ρmat. They can be huge as well as perhaps small—and non-metallic (no elements except hydrogen and helium). This was the period in the evolution of the early universe immediately after electroweak symmetry breaking, when the fundamental interactions of gravitation, electromagnetism, the strong interaction and the weak interaction had taken their present forms, but the temperature of the universe was still too high to allow quarks to bind together to form hadrons. The singularity from the FLRW metric is interpreted to mean that current theories are inadequate to describe what actually happened at the start of the Big Bang itself.

By far the most accepted understanding is that this is due to an unknown form of energy which has been given the name "dark energy". In contrast, the redshift of very distant objects—radio galaxies and quasars—is an awesome phenomenon; some appear to be moving away at greater than 90 percent of the speed of light.

Thus, to imagine a Universe that is mechanically regulated like some sort of perfect clock is the farthest thing from reality. On a large scale, the Universe we can now contemplate with our telescopes appears to be a little more that 13,000 million years old, and enormously empty. The earliest structures to form are the first stars (known as Population III stars), dwarf galaxies, and quasars (which are thought to be bright, early active galaxies containing a supermassive black hole surrounded by an inward-spiralling accretion disk of gas). (In other words, that there was a beginning to the universe.) Those models do not even call for more than three dimensions, despite the fact that some theories, such as “string theory,” call for a few more. A galaxy emits or absorbs some wavelengths of light more strongly than others. Therefore, in inflationary cosmology, the earliest meaningful time "after the Big Bang" is the time of the end of inflation.

[35][36], The amounts of each light element in the early universe can be estimated from old galaxies, and is strong evidence for the Big Bang. According to traditional Big Bang cosmology, the electroweak epoch began 10−36 seconds after the Big Bang, when the temperature of the universe was low enough (1028 K) for the electronuclear force to begin to manifest as two separate interactions, the strong and the electroweak interactions. This indicates that, in finding the intersection, one should not neglect the curvature term in the general equation of the expanding universe.

Which of them will happen, if any, depends on the precise values of physical constants such as the cosmological constant, the possibility of proton decay, the energy of the vacuum (meaning, the energy of "empty" space itself), and the natural laws beyond the Standard Model. These clumps, which had seeds in the fluctuations in the CMB spectrum (shown in Figure 3), were denser than their surroundings by only about one part in 100,000.

When they compared the data they obtained with those galaxies’ red shift—which measures the expansion of the Universe—they were surprised to discover that, the further away the galaxies, the slower the rate of expansion. [66] More recent observations have shown these ages to be shorter than previously indicated. Today, the Universe continues to expand. /

[63] (This age estimate is now believed to be slightly overstated).[64]. Based upon the emerging science of nucleocosmochronology, the Galactic thin disk of the Milky Way is estimated to have been formed 8.8 ± 1.7 billion years ago.[6]. This article was originally published with the title "The Evolution of the Universe" in Scientific American 271, 4, 52-57 (October 1994).

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There is overwhelming evidence that dark matter exists and dominates our universe, but since the exact nature of dark matter is still not understood, the Big Bang theory does not presently cover any stages in its formation.

As our capacity to “see” farther and in more detail has grown, our idea of the Cosmos has changed, and that change has been dramatic in recent times (fig. [43] This process is relatively fast (and faster for the helium than for the hydrogen), and is known as recombination. Extended sample", "BICEP2 March 2014 Results and Data Products", "NASA Technology Views Birth of the Universe", "Space Ripples Reveal Big Bang's Smoking Gun", "Astronomers Hedge on Big Bang Detection Claim", "Cosmic inflation: Confidence lowered for Big Bang signal", "Gravitational Waves from Early Universe Remain Elusive", "Speck of Interstellar Dust Obscures Glimpse of Big Bang", "The Foreground of Big Bang Nucleosynthesis", "Cosmic Neutrinos Detected, Confirming The Big Bang's Last Great Prediction", "Gravitationally Collapsed Objects of Very Low Mass", Monthly Notices of the Royal Astronomical Society, "Thermal history of the universe and early growth of density fluctuations", Harvard–Smithsonian Center for Astrophysics, "Astronomy 162 — Lecture 44: The First Three Minutes", The Astrophysical Journal Supplement Series, Journal of Cosmology and Astroparticle Physics, "Astronomers Finally Spot Universe's First Molecule in Distant Nebula", "New 'Baby Picture' of Universe Unveiled", "Quasars illustrate dark energy's roller coaster ride", "Searching for First Light in the Early Universe", "Much-Discussed Views That Go Way Back - Avi Loeb Ponders the Early Universe, Nature and Life", "First stars formed even later than we thought", "Hubble Team Breaks Cosmic Distance Record (03/03/2016) - Fast Facts", "Ancient Galaxy May Be Most Distant Ever Seen", Publications of the Astronomical Society of Australia, "Illuminating illumination: what lights up the universe? At this moment, matter, energy, space and time did not exist. Distant galaxies also present those local dynamic effects, but from our enormously distant perspective, they are overshadowed by their great recession speeds. The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative

Ordinary matter, which can lose energy by radiation, forms dense objects and also gas clouds when it collapses. In order to get a, universe (which was the accepted viewn 1917 when the theory was first published), he introduced a “fudge factor”, the “cosmological constant”, to cancel out the effects of gravity. It is somewhat misleading, however, to describe the expansion as some type of explosion of matter away from some particular point in space. Big Crunch will produce a new Big Bang and the process Moreover, we are designed to be curious.

(No observation we have made allows us to look back beyond the moment at which the expansion began.) In this kind of extreme timescale, extremely rare quantum phenomena may also occur that are extremely unlikely to be seen on a timescale smaller than trillions of years. Between about 2 and 20 minutes after the Big Bang, the temperature and pressure of the universe allowed nuclear fusion to occur, giving rise to nuclei of a few light elements beyond hydrogen ("Big Bang nucleosynthesis"). *Your comment will be reviewed before being published. The chronology of the universe describes the history and future of the universe according to Big Bang cosmology. From about 9.8 billion years of cosmic time,[7] the universe's large-scale behaviour is believed to have gradually changed for the third time in its history. First we should remember that, in keeping with what we have already said, more than three quarters of our Cosmos is now a form of that mysterious entity we call dark energy, and more than 85% of the rest is what is called “dark matter,” which we cannot see because, though it interacts with gravity, it does not interact with radiation. Much has been written about time’s arrow, trying to discover where the evolution of our Universe is headed and, since it had a beginning, finding out what its end will be. If supersymmetry is a property of our universe, then it must be broken at an energy that is no lower than 1 TeV, the electroweak scale. The Standard Model of cosmology attempts to explain how the universe physically developed once that moment happened. Gravitational attraction also gradually pulls galaxies towards each other to form groups, clusters and superclusters. Even though such a region is subject to overall expansion, the excess of matter leads it to contract, creating a linked object, which may be a star, a stellar cumulus, or a galaxy. Advances in particle physics suggest some interesting ways these questions might be answered; the challenge is to find experimental tests of the ideas. In the case of indefinitely continuing metric expansion of space, the energy density in the universe will decrease until, after an estimated time of 10, Expansion of space accelerates and at some point becomes so extreme that even subatomic particles and the fabric of, For any value of the dark energy content of the universe where the negative pressure ratio is less than -1, the expansion rate of the universe will continue to increase without limit. (or is it just me...), Smithsonian Privacy However, the intersection point ρmat. They can be huge as well as perhaps small—and non-metallic (no elements except hydrogen and helium). This was the period in the evolution of the early universe immediately after electroweak symmetry breaking, when the fundamental interactions of gravitation, electromagnetism, the strong interaction and the weak interaction had taken their present forms, but the temperature of the universe was still too high to allow quarks to bind together to form hadrons. The singularity from the FLRW metric is interpreted to mean that current theories are inadequate to describe what actually happened at the start of the Big Bang itself.

By far the most accepted understanding is that this is due to an unknown form of energy which has been given the name "dark energy". In contrast, the redshift of very distant objects—radio galaxies and quasars—is an awesome phenomenon; some appear to be moving away at greater than 90 percent of the speed of light.

Thus, to imagine a Universe that is mechanically regulated like some sort of perfect clock is the farthest thing from reality. On a large scale, the Universe we can now contemplate with our telescopes appears to be a little more that 13,000 million years old, and enormously empty. The earliest structures to form are the first stars (known as Population III stars), dwarf galaxies, and quasars (which are thought to be bright, early active galaxies containing a supermassive black hole surrounded by an inward-spiralling accretion disk of gas). (In other words, that there was a beginning to the universe.) Those models do not even call for more than three dimensions, despite the fact that some theories, such as “string theory,” call for a few more. A galaxy emits or absorbs some wavelengths of light more strongly than others. Therefore, in inflationary cosmology, the earliest meaningful time "after the Big Bang" is the time of the end of inflation.

[35][36], The amounts of each light element in the early universe can be estimated from old galaxies, and is strong evidence for the Big Bang. According to traditional Big Bang cosmology, the electroweak epoch began 10−36 seconds after the Big Bang, when the temperature of the universe was low enough (1028 K) for the electronuclear force to begin to manifest as two separate interactions, the strong and the electroweak interactions. This indicates that, in finding the intersection, one should not neglect the curvature term in the general equation of the expanding universe.

Which of them will happen, if any, depends on the precise values of physical constants such as the cosmological constant, the possibility of proton decay, the energy of the vacuum (meaning, the energy of "empty" space itself), and the natural laws beyond the Standard Model. These clumps, which had seeds in the fluctuations in the CMB spectrum (shown in Figure 3), were denser than their surroundings by only about one part in 100,000.

When they compared the data they obtained with those galaxies’ red shift—which measures the expansion of the Universe—they were surprised to discover that, the further away the galaxies, the slower the rate of expansion. [66] More recent observations have shown these ages to be shorter than previously indicated. Today, the Universe continues to expand. /

[63] (This age estimate is now believed to be slightly overstated).[64]. Based upon the emerging science of nucleocosmochronology, the Galactic thin disk of the Milky Way is estimated to have been formed 8.8 ± 1.7 billion years ago.[6]. This article was originally published with the title "The Evolution of the Universe" in Scientific American 271, 4, 52-57 (October 1994).

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