A potential energy threshold that particles must overcome, here tunneled through by electrons.An energy barrier is a potential energy threshold that a particle must overcome to transition from one state to another. In classical physics, a particle needs kinetic energy at least equal to the barrier height to pass over it. In quantum mechanics, however, particles can 'tunnel' through barriers even with less energy, a purely wave-like phenomenon with no classical analogue. This concept is central to nuclear fusion in stars, where protons tunnel through the Coulomb repulsion to fuse, and to many electronic devices.
The concept emerged in the late 1920s when George Gamow, and independently Ronald Gurney and Edward Condon, used quantum tunneling to explain alpha decay — the first application of quantum mechanics to nuclear physics.
A particle approaching a barrier is described by a wavefunction that penetrates into the classically forbidden region. If the barrier is thin enough, the wavefunction's amplitude does not decay to zero before reaching the other side, giving a small but nonzero probability of transmission. The tunneling probability depends exponentially on the barrier's width and height, as well as the particle's mass — lighter particles tunnel more easily. This is why electrons tunnel readily in semiconductors, while heavier nuclei require extremely thin barriers.
Tunneling through energy barriers is exploited in flash memory storage, scanning tunneling microscopes that image surfaces atom by atom, and in the design of tunnel diodes for high-speed electronics.
The Sun's fusion reactions proceed at a rate that would be impossible classically — the core temperature is too low for protons to overcome the Coulomb barrier — but quantum tunneling makes it happen, and the Sun shines because of it.








