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Nuclear fusion occurs when two nuclei fuse together. This is frequently nuclei of deuterium and tritium (both hydrogen isotopes), which form a helium nucleus plus a neutron.
The helium flash converts helium nuclei into carbon nuclei through the fusion process in the core of a star. This process occurs in stars with a mass greater than about 0.8 times the mass of the Sun during the later stages of helium burning. The intense energy released during the helium flash helps stabilize the star against gravitational collapse.
The process is called fusion; hydrogen nuclei are fused together to make helium. At much higher temperatures and pressures, the helium can fuse into carbon and nitrogen and oxygen.
Carbon, mainly. Two helium nuclei make beryllium-8, which normally decays practically instantaneously back into the helium nuclei, but if a third helium nucleus hits it first it will make the stable carbon-12. More helium can then be added to make oxygen, neon, magnesium, silicon, sulfur, argon, calcium, titanium, chromium, iron, and finally nickel before the process becomes endergonic.
The next nuclear fusion cycle after helium fusion in a massive star is carbon fusion. This process involves fusing helium nuclei to form carbon. Carbon fusion typically occurs in the core of a massive star after helium fusion is completed.
Three helium nuclei, also known as alpha particles, fuse together to form a carbon atom in the process of stellar nucleosynthesis.
Nuclear fusion occurs when two nuclei fuse together. This is frequently nuclei of deuterium and tritium (both hydrogen isotopes), which form a helium nucleus plus a neutron.
When hydrogen nuclei fuse together, they can form helium. This fusion process is the energy source for stars, including our sun, where hydrogen nuclei combine to form helium through a series of nuclear reactions.
The helium flash converts helium nuclei into carbon nuclei through the fusion process in the core of a star. This process occurs in stars with a mass greater than about 0.8 times the mass of the Sun during the later stages of helium burning. The intense energy released during the helium flash helps stabilize the star against gravitational collapse.
When the nuclei of hydrogen and lithium are fused together, helium is produced.
The process is called fusion; hydrogen nuclei are fused together to make helium. At much higher temperatures and pressures, the helium can fuse into carbon and nitrogen and oxygen.
Hydrogen nuclei (protons) fuse together and produce helium nuclei
Carbon, mainly. Two helium nuclei make beryllium-8, which normally decays practically instantaneously back into the helium nuclei, but if a third helium nucleus hits it first it will make the stable carbon-12. More helium can then be added to make oxygen, neon, magnesium, silicon, sulfur, argon, calcium, titanium, chromium, iron, and finally nickel before the process becomes endergonic.
hydrogen nuclei join together to make a larger helium.
During the solar nuclear reaction, in the proton-proton chain, four hydrogen nuclei (protons) bond together to form a helium nucleus. Two protons combine to form a deuterium nucleus, which then fuses with another proton to form helium-3. Two of the helium-3 nuclei then fuse to form helium-4.
During the solar nuclear reaction, hydrogen nuclei (protons) bond together to form helium nuclei through a process called nuclear fusion. This fusion involves the conversion of hydrogen into helium, releasing a large amount of energy in the form of light and heat.
B- particles are electrons. They are not Helium nuclei.