<p>Stan has essentially answered this in his comment, which I will attempt to spell out a little more laboriously.</p>

<p>The significant majority of our Sun's energy output comes from the <a href="http://en.wikipedia.org/wiki/Proton%E2%80%93proton_chain_reaction" rel="noreferrer">proton-proton chain</a>.  This was advocated by Eddington back in the 1920's, but at that time your basic concern was a very real and major problem.  Objects with like electrical charges repel each other.  In particular, protons will repel other protons since all protons have a positive charge.  What they knew of the sun then indicated that the core was far too cold for protons to overcome this repulsion&mdash;at least not even remotely close to the rate that was obviously necessary to produce a brightly shining sun.</p>

<p>With the development of quantum mechanics it was determined that a process known as <a href="http://en.wikipedia.org/wiki/Quantum_tunnelling" rel="noreferrer">quantum tunneling</a> would give two protons a non-zero probability of "overcoming" this repulsion.  But not in the sense of they just suddenly gain enough energy (hence why "overcoming" is in quotations).  Instead, in the sense that the "fused together" state has the same energy as the "just about to repel each other before fusion can occur" state, and they just randomly switched from the latter to the former, despite every intermediate stage between the two of them requiring more energy than is available.  That this is possible is one of the many non-intuitive features of quantum mechanics, and I think it would be beyond the scope of this question (and site) to try to get much more precise.</p>

<p>Still, even this failed to explain why our sun was very obviously fusing atoms to the extent that it was.  If you fuse two protons together, you are left with an incredibly unstable state: the diproton.  As soon as one of these forms it pretty much immediately breaks up into two distinct protons.</p>

<p>In the late 30's Hans Bethe (a man who eventually won the Nobel prize and was a part of the Los Alamos team that developed the atom bomb) proposed that yet another random quantum mechanical event would save the day: <a href="http://en.wikipedia.org/wiki/Beta_decay" rel="noreferrer">beta decay</a>, a feature of the recently discovered fundamental force known as the <a href="http://en.wikipedia.org/wiki/Weak_interaction" rel="noreferrer">weak force</a>.  In this situation one of the protons in the diproton undergoes a beta decay into a neutron before the diproton separates, at which point you have a stable deuterium nucleus: one proton, and one neutron.</p>

<p>That so many unlikely events have to occur for two protons to produce one deuterium is the reason why the sun's lifetime is approximately 10 billion years.  That the sun shines as bright as it does is, as you suggest, a sheer numbers game: there are truly prodigious numbers of protons in the sun's core, so even though the proton-proton chain is really unlikely, we have so very many chances at it that there is a great many successful fusion events.</p>

<p>Basically every other stellar fusion reaction proceeds much more rapidly than those that produce deuterium.  You may be familiar with the <a href="http://en.wikipedia.org/wiki/Thermonuclear_weapon" rel="noreferrer">hydrogen bomb</a>, which fuses its fuel very rapidly.  One of the key differences (and there are many) between the hydrogen bomb and a star like our sun is that the bomb is fusing together deuterium (and tritium) into helium, and is not using the proton-proton chain.  Stars have to produce large supplies of deuterium directly, and this is a lengthy process that consumes roughly 90% of a star's life&mdash;even for very massive stars, whose lifespans are orders of magnitude shorter than our Sun's.  </p>

<p>(Note that very massive stars are rather more complicated beasts, in fact, but this is again beyond the scope of this question)</p>

CC BY-SA 3.0
2018-02-06T12:37:10.407Z
"*even though the proton-proton chain is really unlikely, we have so very many chances at it that there is a great many successful fusion events.*" This is also why *someone* wins the lottery, even though the odd of winning are so vanishingly small: lots of people play it.
RonJohn
CC BY-SA 4.0
2020-03-31T07:10:50.907Z
It should be noted that stars also use the CNO cycle to produce helium from hydrogen, which doesn't depend on the very tiny chance of converting a diproton into deuterium. This isn't a big contributor in our Sun (and completely negligible in a red dwarf or such), but it's very much in effect for significantly more massive stars - and part of the reason why they last so much shorter than the Sun (the temperature dependency for the CNO cycle is much higher than for the p-p chain).
Luaan
CC BY-SA 4.0
2020-04-01T00:29:02.450Z
@Luaan The question is specifically about the sun, so no, it does not need to be noted.
zibadawa timmy
CC BY-SA 3.0
2015-04-12T11:52:28.867Z
One could add maybe the mention of the Gamow Peak, http://nu.phys.laurentian.ca/~fleurot/fusionrate/  which quantifies the statements made above. Also Deuterium burning already happens in Giant Planets / Brown dwarves that are less massive than the sun.
AtmosphericPrisonEscape
CC BY-SA 3.0
2015-04-12T07:00:44.060Z
2015-04-12T07:00:44.060Z
zibadawa timmy
<p>I recently heard in a discussion that the sun is not massive enough to self-ignite via core-pressure. It simply has not enough mass to "generate" the gravitational force needed for that.</p>

<p>The reason why the sun is still burning is that there is a really small chance that two Hydrogen-Atoms fuse without needing the activation-energy/the activation-energy being provided by a random effect like High-Energy-Particles. Even though the chance is really low, there are so many Hydrogen-Atoms that overall the chance is actually high (law of big numbers). Once some fusion started it provides enough energy to fusion more Hydrogen, leading to our sun shining.</p>

<hr>

<p>The person who presented it only stated that there are sources, but sadly the ones I found from his material didn't support this (nor did they deny it). The sources where about other topic related to stars. I can't ask the person himself as he already changed the university.</p>

CC BY-SA 4.0
2020-07-05T16:48:01.237Z
nitpick: I think law of big/large numbers is not appropriately used here.
NoSenseEtAl
CC BY-SA 3.0
2015-04-12T02:06:35.253Z
Sounds like a somewhat garbled explanation of quantum tunneling through the Coulomb barrier, which is a probabilistic effect that, in this case, allows fusion at lower energies than would be required without tunneling. Regardless, it's plainly not true that the Sun is too small to self-ignite, and it does actually have sufficient gravity.
Stan Liou
CC BY-SA 3.0
2015-04-12T03:08:22.490Z
For fusion to occur either you have high enough temperature sadly the temperature at Sun's core isn't meeting the requirement or you have the hydrogen nucleus which consist on 1 proton and 1 neutron to be near to another hydrogen nucleus. However note that the net charge of a hydrogen nucleus is positive and so repel each other (see coulomb barrier) unless the Sun's gravitational force can bring these hydrogen nucleus near enough so it is possible for one to tunnel through and fusion process begins (see quantum tunneling) I'm just rephrasing Stan Liou's comment for dummies.
user6760
CC BY-SA 3.0
2015-04-12T09:05:28.383Z
The Sun **did** self-ignite; it happened 4.6 billion years ago.
David Hammen
CC BY-SA 3.0
2015-04-12T12:40:26.593Z
@David Hammen No one can *prove* that there wasn't a Bic lighter involved: http://en.wikipedia.org/wiki/Russell%27s_teapot
Wayfaring Stranger
<star><the-sun><hydrogen>
Is the sun too small to self-ignite?
JFBM
# Is the sun too small to self-ignite?

(Asked by: username_0 on 2015-04-12)

I recently heard in a discussion that the sun is not massive enough to self-ignite via core-pressure. It simply has not enough mass to "generate" the gravitational force needed for that.

The reason why the sun is still burning is that there is a really small chance that two Hydrogen-Atoms fuse without needing the activation-energy/the activation-energy being provided by a random effect like High-Energy-Particles. Even though the chance is really low, there are so many Hydrogen-Atoms that overall the chance is actually high (law of big numbers). Once some fusion started it provides enough energy to fusion more Hydrogen, leading to our sun shining.

---

The person who presented it only stated that there are sources, but sadly the ones I found from his material didn't support this (nor did they deny it). The sources where about other topic related to stars. I can't ask the person himself as he already changed the university.

**Tags:** star, the-sun, hydrogen
> **Comments:**
> **username_2**: Sounds like a somewhat garbled explanation of quantum tunneling through the Coulomb barrier, which is a probabilistic effect that, in this case, allows fusion at lower energies than would be required without tunneling. Regardless, it's plainly not true that the Sun is too small to self-ignite, and it does actually have sufficient gravity.  
> **username_3**: For fusion to occur either you have high enough temperature sadly the temperature at Sun's core isn't meeting the requirement or you have the hydrogen nucleus which consist on 1 proton and 1 neutron to be near to another hydrogen nucleus. However note that the net charge of a hydrogen nucleus is positive and so repel each other (see coulomb barrier) unless the Sun's gravitational force can bring these hydrogen nucleus near enough so it is possible for one to tunnel through and fusion process begins (see quantum tunneling) I'm just rephrasing Stan Liou's comment for dummies.  
> **username_4**: The Sun **did** self-ignite; it happened 4.6 billion years ago.  
> **username_5**: @David Hammen No one can *prove* that there wasn't a Bic lighter involved: http://en.wikipedia.org/wiki/Russell%27s_teapot  
> **username_1**: nitpick: I think law of big/large numbers is not appropriately used here.  

---

## 1 answers

### Answer by username_6 on 2015-04-12. Score: 7 | Accepted answer

Stan has essentially answered this in his comment, which I will attempt to spell out a little more laboriously.

The significant majority of our Sun's energy output comes from the [proton-proton chain](http://en.wikipedia.org/wiki/Proton%E2%80%93proton_chain_reaction). This was advocated by Eddington back in the 1920's, but at that time your basic concern was a very real and major problem. Objects with like electrical charges repel each other. In particular, protons will repel other protons since all protons have a positive charge. What they knew of the sun then indicated that the core was far too cold for protons to overcome this repulsion—at least not even remotely close to the rate that was obviously necessary to produce a brightly shining sun.

With the development of quantum mechanics it was determined that a process known as [quantum tunneling](http://en.wikipedia.org/wiki/Quantum_tunnelling) would give two protons a non-zero probability of "overcoming" this repulsion. But not in the sense of they just suddenly gain enough energy (hence why "overcoming" is in quotations). Instead, in the sense that the "fused together" state has the same energy as the "just about to repel each other before fusion can occur" state, and they just randomly switched from the latter to the former, despite every intermediate stage between the two of them requiring more energy than is available. That this is possible is one of the many non-intuitive features of quantum mechanics, and I think it would be beyond the scope of this question (and site) to try to get much more precise.

Still, even this failed to explain why our sun was very obviously fusing atoms to the extent that it was. If you fuse two protons together, you are left with an incredibly unstable state: the diproton. As soon as one of these forms it pretty much immediately breaks up into two distinct protons.

In the late 30's Hans Bethe (a man who eventually won the Nobel prize and was a part of the Los Alamos team that developed the atom bomb) proposed that yet another random quantum mechanical event would save the day: [beta decay](http://en.wikipedia.org/wiki/Beta_decay), a feature of the recently discovered fundamental force known as the [weak force](http://en.wikipedia.org/wiki/Weak_interaction). In this situation one of the protons in the diproton undergoes a beta decay into a neutron before the diproton separates, at which point you have a stable deuterium nucleus: one proton, and one neutron.

That so many unlikely events have to occur for two protons to produce one deuterium is the reason why the sun's lifetime is approximately 10 billion years. That the sun shines as bright as it does is, as you suggest, a sheer numbers game: there are truly prodigious numbers of protons in the sun's core, so even though the proton-proton chain is really unlikely, we have so very many chances at it that there is a great many successful fusion events.

Basically every other stellar fusion reaction proceeds much more rapidly than those that produce deuterium. You may be familiar with the [hydrogen bomb](http://en.wikipedia.org/wiki/Thermonuclear_weapon), which fuses its fuel very rapidly. One of the key differences (and there are many) between the hydrogen bomb and a star like our sun is that the bomb is fusing together deuterium (and tritium) into helium, and is not using the proton-proton chain. Stars have to produce large supplies of deuterium directly, and this is a lengthy process that consumes roughly 90% of a star's life—even for very massive stars, whose lifespans are orders of magnitude shorter than our Sun's.

(Note that very massive stars are rather more complicated beasts, in fact, but this is again beyond the scope of this question)

> **Comments:**
> **username_9**: One could add maybe the mention of the Gamow Peak, http://nu.phys.laurentian.ca/~fleurot/fusionrate/  which quantifies the statements made above. Also Deuterium burning already happens in Giant Planets / Brown dwarves that are less massive than the sun.  
> **username_7**: "*even though the proton-proton chain is really unlikely, we have so very many chances at it that there is a great many successful fusion events.*" This is also why *someone* wins the lottery, even though the odd of winning are so vanishingly small: lots of people play it.  
> **username_8**: It should be noted that stars also use the CNO cycle to produce helium from hydrogen, which doesn't depend on the very tiny chance of converting a diproton into deuterium. This isn't a big contributor in our Sun (and completely negligible in a red dwarf or such), but it's very much in effect for significantly more massive stars - and part of the reason why they last so much shorter than the Sun (the temperature dependency for the CNO cycle is much higher than for the p-p chain).  
> **username_6**: @Luaan The question is specifically about the sun, so no, it does not need to be noted.  

---

