6 H --> He + 2 H
There are several intermediate steps omitted.
4 nuclei
Two protons would be particle unstable, so one of them must change to a neutron. This will always produce a deuteron, a positron and an (electron)neutrino and a gamma ray will be emitted. This is true for the simple p-p chain which is predominant in the Sun, and also in the CNO cycle which is a minor component of the Sun's fusion but important for more massive stars.
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In a fission reaction, energy is released when a heavy nucleus splits into lighter nuclei and neutrons. In a fusion reaction, energy is released when light nuclei combine to form a heavier nucleus. Both reactions release a large amount of energy due to the difference in binding energy between the initial and final nuclei.
The cores of stars, such as our sun, have high enough temperatures and pressures to enable fusion of hydrogen nuclei - it is very difficult to fuse these positively charged particle together without these conditions. The mass of the nuclei before fusion is greater than the final mass of the fused particles - some of the mass is converted directly into energy through Einsteins equation E=mc2. m represents the mass, which although very small, is multiplied by the speed of light squared (c2), which is a very large number.
Through nuclear fusion, where smaller atoms are fused together to make larger atoms under extreme pressures and temperatures. Usually hydrogen nuclei are being fused together to make helium nuclei. The total mass of the components is more than the final helium nuclei, the excess mass is turned into energy (E=MC^2). Massive amounts of energy are released through this process.
Helium is converted to carbon in the final stage of fusion in stars like the Sun, which are considered to be medium-sized stars. This happens during the triple-alpha process where three helium nuclei combine to form a carbon nucleus.
in a protostar before fusion ignites, gravity.in a normal star, fusion.in a star at the end of its life when fusion burns out, gravity. This is what drives the final blast of a supernova explosion.
During the fusion process, mass is converted into energy through the combination of atomic nuclei to form a heavier nucleus. This process releases a large amount of energy in the form of electromagnetic radiation, such as gamma rays. The energy released is a result of the difference in mass between the initial nuclei and the final nucleus, as described by Einstein's famous equation, Emc2.
The nuclear reactors we have now are fission reactors. This means that they obtain their energy from nuclear reactions that split large nuclei such as uranium into smaller ones such as rubidium and cesium. There is a binding energy that holds a nucleus together. If the binding energy of the original large nucleus is greater than the sum of the binding energies of the smaller pieces, you get the difference in energy as heat that can be used in a power station to generate electricity. A fusion reaction works the other way. It takes small nuclei like deuterium (heavy hydrogen) and fuses them together to make larger ones such as helium. If the binding energy of the two deuterium nuclei is greater than that of the final larger helium nucleus, it can be used to generate electricity. There are two main differences between fission and fusion. The first is that the materials required for fission are rarer and more expensive to produce than those for fusion. For example, uranium has to be mined in special areas and then purified by difficult processes. By contrast, even though deuterium makes up only 0.02 percent of naturally occurring hydrogen, we have a vast supply of hydrogen in the water making up the oceans. The second difference is that the products of fission are radioactive and so need to be treated carefully, as they are dangerous to health. The products of fusion are not radioactive (although a realistic reactor will likely have some relatively small amount of radioactive product). The problem with building fusion reactors is that a steady, controlled fusion reaction is very hard to achieve. It is still a subject of intense research. The main problem is that to achieve fusion we need to keep the nuclei we wish to fuse at extremely high temperatures and close enough for them to have a chance of fusing with one other. It is extremely difficult to find a way of holding everything together, since the nuclei naturally repel each other and the temperatures involved are high enough to melt any solid substance known. As technology improves, holding everything together will become easier, but it seems that we are a long way off from having commercial fusion reactors.
The Omega Metroid.
Proteins are the final product. They are made from amino acids.