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Attribution:
Up and Atom
Arvin Ash
video chapter:
00:00 - intro about quantum tunneling
00:35 - what is quantum tunneling
05:35 - Is it possible for a human to quantum tunneling?
06:27 - quantum tunneling in sun
07:40 - quantum tunneling in DNA
07:50 - quantum tunneling in transistors
Quantum tunnelling or tunneling is the quantum mechanical phenomenon where a wave function can propagate through a potential barrier. The transmission through the barrier can be finite and depends exponentially on the barrier height and barrier width. The wave function may disappear on one side and reappear on the other side. The wave function and its first derivative are continuous. In steady-state, the probability flux in the forward direction is spatially uniform. No particle or wave is lost. Tunneling occurs with barriers of thickness around 1-3 nm and smaller.
Quantum tunneling is not predicted by the laws of classical mechanics where surmounting a potential barrier requires potential energy.Tunneling may be explained in terms of the Heisenberg uncertainty principle in that a quantum object can be known as a wave or as a particle in general. In other words, the uncertainty in the exact location of light particles allows these particles to break rules of classical mechanics and move in space without passing over the potential energy barrier.
Quantum tunneling plays an essential role in physical phenomena, such as nuclear fusion.It has applications in the tunnel diode,quantum computing, and in the scanning tunneling microscope.
Quantum tunneling is projected to create physical limits to the size of the transistors used in microelectronics, due to electrons being able to tunnel past transistors that are too small.
Quantum tunneling is an essential phenomenon for nuclear fusion. The temperature in stars' cores is generally insufficient to allow atomic nuclei to overcome the Coulomb barrier and achieve thermonuclear fusion. Quantum tunneling increases the probability of penetrating this barrier. Though this probability is still low, the extremely large number of nuclei in the core of a star is sufficient to sustain a steady fusion reaction.
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