Nuclear fusion occurs when
nuclei,
protons and
neutrons, come close enough together for the
nuclear force to pull them together into a single larger nucleus. Opposing this action is the
electrostatic force, which causes electrically charged particles with like charges, like protons, to repel each other. To fuse, the particles must be travelling fast enough to overcome this
coulomb barrier. The nuclear force increases with the number of nuclei, and the coulomb barrier is lowered when the number of neutrons in the nuclei is maximized, which leads to the fusion rate being maximized for
isotopes of lighter elements like
hydrogen and
helium with extra neutrons. Using classical
electromagnetism, the energies required to overcome the coulomb barrier would be enormous. The calculations changed considerably during the 1920s as physicists explored the new science of
quantum mechanics.
George Gamow's 1928 paper on
quantum tunnelling demonstrated that nuclear reactions could take place at much lower energies than classical theory predicted. Using this new theory, in 1929
Fritz Houtermans and
Robert Atkinson demonstrated that expected reaction rates in the core of the sun supported
Arthur Eddington's 1920 suggestion that the sun is powered by fusion. In 1934,
Mark Oliphant,
Paul Harteck and
Ernest Rutherford were the first to achieve fusion on Earth, using a
particle accelerator to shoot
deuterium nuclei into a metal foil containing deuterium,
lithium and other elements. This allowed them to measure the
nuclear cross section of various fusion reactions, and determined that the deuterium-deuterium reaction occurred at the lowest energy, peaking at about 100,000
electronvolts (100 keV). This energy corresponds to the average energy of particles in a gas heated to about 10 billion
Kelvin (K). Materials heated beyond a few thousand K dissociate into their
electrons and
nuclei, producing a gas-like
state of matter known as
plasma. In any gas the particles have a wide range of energies, normally following the
Maxwell–Boltzmann statistics. In such a mixture, a small number of particles will have much higher energy than the bulk. This leads to an interesting possibility; even at average temperatures well below 100 keV, some particles within the gas will randomly have enough energy to undergo fusion. Those reactions release huge amounts of energy. If that energy can be captured back into the plasma, it can heat other particles to that energy as well, making the reaction self-sustaining. In 1944,
Enrico Fermi calculated this would occur at about 50 million K for a deuterium-tritium fuel. Taking advantage of this possibility requires the fuel plasma to be held together long enough that these random reactions have time to occur. Like any hot gas, plasma has an internal
pressure and thus wants to expand according to the
ideal gas law. For a fusion reactor, the problem is keeping the plasma contained against this pressure; any known substance would melt at these temperatures. As it consists of freely moving charged particles, plasma is
electrically conductive. This makes it subject to electric and magnetic fields. In a magnetic field, the electrons and nuclei orbit the magnetic field lines. A simple confinement system is a plasma-filled tube placed inside the open core of a
solenoid. The plasma naturally wants to expand outwards to the walls of the tube, as well as move along it, towards the ends. The solenoid creates a magnetic field running down the centre of the tube, which the particles will orbit, preventing their motion towards the sides. Unfortunately, this arrangement does not confine the plasma along the length of the tube, and the plasma is free to flow out the ends. For a purely experimental machine, the losses are not necessarily a major problem, but a production system would have to eliminate these end losses. ==Pinch effect==