wookiemeister said:
wouldn’t protons repel each other too, not only electrons?
if you had an errant proton floating around it would repel another proton I bet
Sure. But you don’t normally get stray protons floating around in normal matter, they’re generally shielded by electrons. The nucleus of an atom is much tinier than the atom’s electron “cloud”, so the inverse square law says that when two atoms are in proximity it’s the electron repulsion that is the important thing.
Of course, in a hydrogen plasma it’s a different story, since there you do have naked protons & electrons flying around.
Dropbear said:
Strong nuclear force > electromagnetic force
Certainly, once the protons are close enough to each other. But it takes a
lot of energy to overcome the electrostatic repulsion to get them that close. Just ask the people who are trying to build fusion reactors. :) Even in the core of a typical star the odds of fusion occurring are pretty low, which is a good thing, otherwise we wouldn’t have stable stars.
From Proton–proton chain reaction
The proton–proton chain reaction is one of several fusion reactions by which stars convert hydrogen to helium, the primary alternative being the CNO cycle. The proton–proton chain dominates in stars the size of the Sun or smaller.
In general, proton–proton fusion can occur only if the temperature (i.e. kinetic energy) of the protons is high enough to overcome their mutual electrostatic or Coulomb repulsion.
In the Sun, deuterium-producing events are so rare (diprotons, the much more common result of nuclear reactions within the star, immediately decay back into two protons) that a complete conversion of the star’s hydrogen would take more than 1010 (ten billion) years at the prevailing conditions of its core. The fact that the Sun is still shining is due to the slow nature of this reaction; if it went more quickly, the Sun would have exhausted its hydrogen long ago.
History of the theory
The theory that proton–proton reactions were the basic principle by which the Sun and other stars burn was advocated by Arthur Stanley Eddington in the 1920s. At the time, the temperature of the Sun was considered too low to overcome the Coulomb barrier. After the development of quantum mechanics, it was discovered that tunneling of the wavefunctions of the protons through the repulsive barrier allows for fusion at a lower temperature than the classical prediction.
Even so, it was unclear how proton–proton fusion might proceed, because the most obvious product, helium-2 (diproton), is unstable and immediately dissociates back into a pair of protons. In 1939, Hans Bethe proposed that one of the protons could beta decay into a neutron via the weak interaction during the brief moment of fusion, making deuterium the initial product in the chain. This idea was part of the body of work in stellar nucleosynthesis for which Bethe won the 1967 Nobel Prize in Physics.