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The Big Bang Theory
The Big Bang theory is the theory of element formation in the early universe. It ended when the universe was about 3 minutes old after its temperature dropped below the fusion temperature. There was a short period of nuclear synthesis during the Big Bang, so the lighter chemical elements were created. Starting with hydrogen ions (protons), which mainly produced deuterium, helium-4 and lithium. Other items were produced in abundance later.
The basic theory of nuclear synthesis was developed in 1948 by George Gamow, Ralph Asher Alvear and Robert Hermann.
This basic theory was used for many years as a study of physics at the time of the Big Bang, as the theory of nuclear synthesis in the Big Bang links the abundance of primordial light elements with elements of the early universe.
The formation and evolution of the vast structure of galaxies
Understanding the formation and evolution of the broader and older structure of galaxies (for example, quasars, galaxy clusters and clusters) is one of the biggest efforts in cosmology. Cosmologists study a model of hierarchical formation in which structures form from the bottom up, with small clusters forming first, while larger clusters such as galaxy clusters are still in the clustering stage. Another tool for understanding structure formation is the simulation that cosmologists use to study the gravitational assembly of matter in The universe, where it collects in strings and then in enormous chains. Most of the simulations contain only cool, non-baryon dark matter, which should be sufficient to fully understand the universe, as there is much more dark matter in the universe than visible and baryonic matter. More advanced simulations have begun to include baryons and the study of the formation of individual galaxies. Cosmologists study this simulation to see if they agree with surveys of galaxies, and in order to understand any anisotropy
Evidence from the nuclear synthesis of the Big Bang, the background of the cosmic microwave radiation and the formation of structures and the curves of the galaxy's rotation indicate that about 23% of the mass of the universe is composed of non-baryonic dark matter while only 4% of it is baryonic visible matter. The side effects of dark matter are well understood, as it behaves like a cold, non-radioactive liquid that forms halos around galaxies. Dark matter has not been discovered in laboratories, and the nature of the particle physics in dark matter remains completely unknown.
If the universe was flat, then there should be an additional component consisting of 73% of the energy density in the universe plus 23% of dark matter and 4% of baryons. This is called dark energy. In order not to interfere with the nuclear synthesis of the Big Bang and the background of the cosmic microwave radiation, it should not coalesce into halos such as baryons and dark matter. There is strong observational evidence for dark energy, as the total energy density of the universe is known through the constraints on the flattening of the universe, but the amount of matter collected is tightly measured, and it is much less than that. H
Additional information for the current page content
The Big Bang Theory
The Big Bang theory is the theory of element formation in the early universe. It ended when the universe was about 3 minutes old after its temperature dropped below the fusion temperature. There was a short period of nuclear synthesis during the Big Bang, so the lighter chemical elements were created. Starting with hydrogen ions (protons), which mainly produced deuterium, helium-4 and lithium. Other items were produced in abundance later.
The basic theory of nuclear synthesis was developed in 1948 by George Gamow, Ralph Asher Alvear and Robert Hermann.
This basic theory was used for many years as a study of physics at the time of the Big Bang, as the theory of nuclear synthesis in the Big Bang links the abundance of primordial light elements with elements of the early universe.
The formation and evolution of the vast structure of galaxies
Understanding the formation and evolution of the broader and older structure of galaxies (for example, quasars, galaxy clusters and clusters) is one of the biggest efforts in cosmology. Cosmologists study a model of hierarchical formation in which structures form from the bottom up, with small clusters forming first, while larger clusters such as galaxy clusters are still in the clustering stage. Another tool for understanding structure formation is the simulation that cosmologists use to study the gravitational assembly of matter in The universe, where it collects in strings and then in enormous chains. Most of the simulations contain only cool, non-baryon dark matter, which should be sufficient to fully understand the universe, as there is much more dark matter in the universe than visible and baryonic matter. More advanced simulations have begun to include baryons and the study of the formation of individual galaxies. Cosmologists study this simulation to see if they agree with surveys of galaxies, and in order to understand any anisotropy
Evidence from the nuclear synthesis of the Big Bang, the background of the cosmic microwave radiation and the formation of structures and the curves of the galaxy's rotation indicate that about 23% of the mass of the universe is composed of non-baryonic dark matter while only 4% of it is baryonic visible matter. The side effects of dark matter are well understood, as it behaves like a cold, non-radioactive liquid that forms halos around galaxies. Dark matter has not been discovered in laboratories, and the nature of the particle physics in dark matter remains completely unknown.
If the universe was flat, then there should be an additional component consisting of 73% of the energy density in the universe plus 23% of dark matter and 4% of baryons. This is called dark energy. In order not to interfere with the nuclear synthesis of the Big Bang and the background of the cosmic microwave radiation, it should not coalesce into halos such as baryons and dark matter. There is strong observational evidence for dark energy, as the total energy density of the universe is known through the constraints on the flattening of the universe, but the amount of matter collected is tightly measured, and it is much less than that. H
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