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The Sun is a main-sequence star, and, as such, generates its energy by nuclear fusion of hydrogen nuclei into helium. In its core, the Sun fuses 620 million metric tons of hydrogen and makes 616 million metric tons of helium each second.
At the Sun's core temperature of 15.5 million K the PP process is dominant. The PP process and the CNO process are equal at around 20 MK. [1] Scheme of the proton–proton branch I reaction. The proton–proton chain, also commonly referred to as the p–p chain, is one of two known sets of nuclear fusion reactions by which stars convert ...
On the sun, where fusion occurs naturally, the strong gravitational pull keeps hydrogen atoms from dispersing. Scientists can do the same thing with magnets, but that comes with another set of ...
Hydrogen fusion (nuclear fusion of four protons to form a helium-4 nucleus [20]) is the dominant process that generates energy in the cores of main-sequence stars. It is also called "hydrogen burning", which should not be confused with the chemical combustion of hydrogen in an oxidizing atmosphere.
Scientists have achieved record breaking temperatures within an ‘artificial sun’ reactor, marking a major advance in the development of nuclear fusion energy.. The new world record saw a ball ...
Learning from the sun. Nuclear fusion occurs when two atoms of a light element such as hydrogen are heated and fused together to form a heavier element such as helium. In order for that process to ...
Diagram showing the Sun's components. The core is where nuclear fusion takes place, creating solar neutrinos. A solar neutrino is a neutrino originating from nuclear fusion in the Sun's core, and is the most common type of neutrino passing through any source observed on Earth at any particular moment.
A nuclear fusion reaction, which is what keeps the sun and other stars burning, occurs when the nuclei of two atoms fuse into one atomic nucleus. When that happens, the excess mass converts into ...