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In what type of star would helium be converted to carbon as the final stage of fusion?
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∙ 10y ago
Brown dwarf
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∙ 10y ago
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What type of star would helium be converted to carbon as the final stage of fusion?
Brown Dwarf
How hydrogen converted into helium in sun.full description?
Comparing the mass of the final helium-4 atom with the masses of the four protons reveals that 0.007 or 0.7% of the mass of the original protons has been lost. This mass has been converted into energy, in the form of gamma rays and neutrinos released during each of the individual reactions. The total energy yield of one whole chain is {{val|26.73|u=MeV}}.
The sun gets its energy from?
the fusion of 4 hydrogen atoms to form 1 helium atom. Fusion of light atoms results in new energy, just as the breaking apart (fission) of heavy atoms does. It happens that iron is the mid-point (i.e. the atom with the least binding energy).
What is the critical temperature at which hydrogen can begin to fuse into helium in the core of a star?
Helium fusion occurs in the core of the stars that are in that stage of life where they have exhausted their hydrogen fuel and begin to burn helium. Wikipedia has some additional information and a link is provided.
What is final core element for a solar like star?
The final elements fused in a star of the mass of our Sun are Oxygen then Carbon. Therefore a white dwarf core could be regarded as a solid, gigantic diamond.
What type of star would helium be converted to carbon as the final stage of fusion?
Brown Dwarf
What type of star would helium be converted to carbon as the final stage or fusion?
red giant (k12)
What type of fusion occurs in a high-mass star near the end stages of its life cycle?
helium capture
How does carbon release energy fusion or fission?
Two carbon-12 nuclei can fuse into a magnesium-24 nucleus in a star with enough pressure and temperature. Two magnesium-24 nuclei can fuse into a chromium-48 nucleus in a star with enough pressure and temperature. Chromium-48 decays by K capture with a half life of 23.5 hours to vanadium-48. Vanadium-48 decays by Beta+ emission or K capture with a half life of 16.1 days to titanium-48. Two titanium-48 nuclei can fuse into a ruthenium-96 nucleus in a star with enough pressure and temperature. In this chain, fusion ends here and the product is stable. In the most typical fusion chain from carbon upward in stars it is more complex and the final product is a mixture of iron and nickel isotopes that are all stable and fusion ends there. The difficulty in getting to carbon in the first place is that helium-helium fusion is a "forbidden" reaction, only the rare helium-helium-helium fusion reaction which is allowed at high enough density, pressure, and temperature can produce carbon. This is the fusion reaction that powers red giant stars and is why they grow so gigantic and their photosphere is so far from the energy source that it cools to red heat.
How hydrogen converted into helium in sun.full description?
Comparing the mass of the final helium-4 atom with the masses of the four protons reveals that 0.007 or 0.7% of the mass of the original protons has been lost. This mass has been converted into energy, in the form of gamma rays and neutrinos released during each of the individual reactions. The total energy yield of one whole chain is {{val|26.73|u=MeV}}.
Who is the final boss of Metroid Fusion?
The Omega Metroid.
What is the percentage nitrogen in the earths atmosphere?
78% of the Earth's atmosphere is Nitrogen. Another 21% is oxygen, and the final 1% are other gases found is small amounts such as carbon dioxide, helium and methane.
What percentage is nitrogen and oxygen in the earth's atmosphere?
78% of the Earth's atmosphere is Nitrogen. Another 21% is oxygen, and the final 1% are other gases found is small amounts such as carbon dioxide, helium and methane.
What happens during nuclear fusion in the stars?
When a star is undergoing nuclear fusion its tremendous gravity is forcing the nuclei of atoms together, releasing extremely large amounts of energy. This release of energy is all that prevents a star from imploding under its own gravity.
The sun gets its energy from?
the fusion of 4 hydrogen atoms to form 1 helium atom. Fusion of light atoms results in new energy, just as the breaking apart (fission) of heavy atoms does. It happens that iron is the mid-point (i.e. the atom with the least binding energy).
Where do stars get there energy from?
Fusion reactions power the stars and produce all but the lightest elements in a process called nucleosynthesis. Although the fusion of lighter elements in stars releases energy, production of elements heavier than iron absorbs energy.When the fusion reaction is a sustained uncontrolled chain, it can result in a thermonuclear explosion, such as that generated by a hydrogen bomb. Reactions which are not self-sustaining can still release considerable energy, as well as large numbers of neutrons.Nucleosynthesis or nucleogenesis is the production of all the chemical elements from the simplest element, hydrogen, by thermonuclear reactions within stars, supernovas, and in the big bang at the beginning of the universe. A star obtains its energy by fusing together light nuclei to form heavier nuclei; in this process, mass (m) is converted into energy (E) in accordance with Einstein's formula, E=mc2, in which cis the speed of light. The reactions are initiated by the high temperatures (about 14 million degrees Celsius) at the center of the star. In the course of producing nuclear energy, the star synthesizes all the elements of the periodic table from its initial composition of mostly hydrogen and a small amount of helium.Transformation of Hydrogen to HeliumThe first step is the fusion of four hydrogen nuclei to make one helium nucleus. This "hydrogen-burning" phase supplies energy to stars on the main sequence of the Hertzsprung-Russell diagram. There are two chains of reactions by which the conversion of hydrogen to helium is effected: the proton-proton cycle and the carbon-nitrogen-oxygen cycle (sometimes referred to simply as the carbon cycle). They were both first studied and proposed as sources of stellar energy by H. Bethe and independently by C. von Weiszäcker. The proton-proton cycle operates in less massive and luminous stars like the sun, while the carbon-nitrogen-oxygen cycle (which speeds up dramatically at higher temperatures) dominates in more massive and luminous stars.The Proton-Proton CycleIn the proton-proton cycle, two hydrogen nuclei (protons) are fused and one of these protons is converted to a neutron by beta decay to make a deuterium nucleus (one proton and one neutron). Then a third proton is added to deuterium to form the light isotope of helium, helium-3. When two helium-3 nuclei collide, they form a nucleus of ordinary helium, helium-4 (two protons and two neutrons), and release two protons. In each of these steps considerable energy is also released.The Carbon-Nitrogen-Oxygen CycleThe carbon-nitrogen-oxygen cycle requires minute traces of carbon as a catalyst. Four protons are added, one by one, to a carbon nucleus to form a succession of excited (unstable) nuclei of carbon, nitrogen, and oxygen. The intermediate nuclei shed their excess electric charge via beta decay and the final oxygen nucleus spontaneously splits into the original carbon nucleus and a helium-4 nucleus, releasing energy. The net effect is again the combination of four hydrogen nuclei to form one helium-4 nucleus; the carbon is free to begin the cycle over again.Creation of the Heavier ElementsAfter the bulk of a star's hydrogen has been converted to helium by either the proton-proton or carbon-nitrogen-oxygen process, the stellar core contracts (while the outer layers expand) until sufficiently high temperatures are reached to initiate "helium-burning" by the triple-alpha process; in this process, three helium nuclei (alpha particles) are fused to make a carbon nucleus. By successive additions of helium nuclei, the heavier elements through iron-56 are built up. The elements whose atomic weights are not multiples of four are created by side reactions that involve neutrons. Because iron-56 is the most stable of the elements, it is very difficult to add an extra helium nucleus to it. However, iron-56 will readily capture a neutron to form the less stable isotope, iron-57. From iron-57, the elements through bismuth-209 can be synthesized. The elements more massive than bismuth-209 are radioactive; that is, they spontaneously break apart. However, during a supernova, an extremely intense flux of neutrons is generated and nuclear reactions proceed so rapidly that the radioactive elements do not have enough time to decay, resulting in the rapid creation of the radioactive elements up to and beyond uranium.
How does helium and hydrogen produce so much energy on the sun?
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.
