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  2. The Hope and Hype of Fusion Energy, Explained - AOL

    www.aol.com/news/hope-hype-fusion-energy...

    Fusion forces together atoms of very light, stable elements like isotopes of hydrogen, creating slightly heavier elements like helium and producing as much as four times as much energy, per unit ...

  3. Fusion power - Wikipedia

    en.wikipedia.org/wiki/Fusion_power

    The heavy nuclei bigger than iron have many more protons resulting in a greater repulsive force. For nuclei lighter than iron-56, the reaction is exothermic, releasing energy when they fuse. Since hydrogen has a single proton in its nucleus, it requires the least effort to attain fusion, and yields the most net energy output. Also since it has ...

  4. National Ignition Facility - Wikipedia

    en.wikipedia.org/wiki/National_Ignition_Facility

    The first large-scale experiments were performed in June 2009 [7] and the first "integrated ignition experiments" (which tested the laser's power) were declared completed in October 2010. [ 8 ] From 2009 to 2012 experiments were conducted under the National Ignition Campaign, with the goal of reaching ignition just after the laser reached full ...

  5. Nuclear fusion - Wikipedia

    en.wikipedia.org/wiki/Nuclear_fusion

    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. The fusion of lighter elements in stars releases energy and the mass that always accompanies it.

  6. Proton–proton chain - Wikipedia

    en.wikipedia.org/wiki/Proton–proton_chain

    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 hydrogen to helium. It dominates in stars with masses less than or equal to that of the Sun , [ 2 ] whereas the CNO cycle , the other known reaction, is suggested by theoretical models to dominate ...

  7. Fusor - Wikipedia

    en.wikipedia.org/wiki/Fusor

    With hydrogen fuels, about 3 to 10 keV is needed to allow the reaction to take place. [ 19 ] Traditional approaches to fusion power have generally attempted to heat the fuel to temperatures where the Maxwell-Boltzmann distribution of their resulting energies is high enough that some of the particles in the long tail have the required energy. [ 19 ]

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  9. Stellar nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Stellar_nucleosynthesis

    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.