Unraveling the Mystery of Proton-Proton Fusion

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In summary: except that if we did include them, we'd get a photon on the right because there would be a free electron and the positron.
  • #1
Artlav
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I've been thinking about nuclear fusion process in the sun, and stumbled upon something weird:

Basically, why there is a net energy from PP fusion?

We have an input of 4 protons and output of 2 protons and 2 neutrons, now, a mass of a neutron is slightly larger than a mass of proton, so the result appears to be more massive, than the input!

Some online research shown that it doesn't go just that simple, but the PP-chain process have the same problem - the input is 6 protons, the output is 2 neutrons and 4 protons, which is again more massive than the input, and above that there are 2 positrons, neutrinos and gamma-quants of net output.

Where does the energy come from?
Kinetic energy of proton collisions?
If yes, what is the point of fusion, if it only reemit parts of the heat that make it go in the first place?

Something does not add up, where am i wrong?
 
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  • #2
I thought one ended up with a He4 nucleus, and not 2p + 2n ;-)

And the mass of He4 is smaller than mass(2p + 2n)
 
  • #3
malawi_glenn said:
I thought one ended up with a He4 nucleus, and not 2p + 2n ;-)

And the mass of He4 is smaller than mass(2p + 2n)

Hm, and He4 nucleus is made out of 2p and 2n, which raises the question, why is it lighter?
Are there different protons and neutrons in the atoms, than in hydrogen and free-flying neutrons?
 
  • #4
This is basic nuclear physics, the mass of the nucleus has lower mass than its constituent particles due to the (negative)binding energy. Same holds for atoms aswell, an atomic nucleus + electrons has higher mass then the atom as a whole.

http://en.wikipedia.org/wiki/Binding_energy

http://hyperphysics.phy-astr.gsu.edu/Hbase/astro/procyc.html

http://en.wikipedia.org/wiki/Nuclear_fusion

http://hyperphysics.phy-astr.gsu.edu/hbase/NucEne/fission.html

Enjoy your reading, if you have any more questions regarding this, please ask hera again :-)
 
  • #5
Thank you for the links, that made some sense although somewhat counter-intuitive at first - energy having "negative mass"...
 
  • #6
While it takes energy to turn a proton into a neutron, there's also energy created when the positron produced from the beta decay of the proton as it turns into a neutron reacts with an electron creating an additional 1.022 MeV of energy. So while you have energy 'left over' when the constituent particles bind to create a larger particle, there's also a little extra from the electron-positron reaction.

http://en.wikipedia.org/wiki/Proton-proton_chain
 
  • #7
Hey,

I'm sorry, could someone please help me to understand the conservation of charge and leptons that happens in the first step of Proton-Proton fusion?

H(1) + H(1) --> H(2) + positron + neutrino. I think I'm missing something to do with an electron? My nucleons balance, but I'm a charge positive and a lepton short on the right hand side of the relation.

thanks.
 
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  • #8
jmgood said:
Hey,

I'm sorry, could someone please help me to understand the conservation of charge and leptons that happens in the first step of Proton-Proton fusion?

H(1) + H(1) --> H(2) + positron + neutrino.


I think I'm missing something to do with an electron? My nucleons balance, but I'm a charge positive and a lepton short on the right hand side of the relation.

thanks.
Charges balance: on left +1 from each H1, on right +1 each from H2 and positron
Lepton balance: positron is antilepton, neutrino is lepton - balance =0.
 
  • #9
mathman said:
Charges balance: on left +1 from each H1, on right +1 each from H2 and positron
Lepton balance: positron is antilepton, neutrino is lepton - balance =0.

So to clarify, we're assuming the atoms are not neutral. Thank you!
 
  • #10
jmgood said:
So to clarify, we're assuming the atoms are not neutral. Thank you!

We're not assuming that; we're just ignoring the electrons because they don't take part in the nuclear reaction we're discussing. If you include them, they'd be on both the left and right sides, so charge still balances.

However, it is actually true that the electrons in the Sun's core are not bound to nuclei. The temperature there is way too high for that.
 
  • #11
ideasrule said:
We're not assuming that; we're just ignoring the electrons because they don't take part in the nuclear reaction we're discussing. If you include them, they'd be on both the left and right sides, so charge still balances.

However, it is actually true that the electrons in the Sun's core are not bound to nuclei. The temperature there is way too high for that.

Okay, I see that. Except that if we did include them, we'd get a photon on the right because there would be a free electron and the positron. Yes? This was the original source of my confusion.
 
  • #12
It's a little appreciated fact but most of the Sun's energy is not from proton-proton fusion at all. That's the underlying source reaction of all the big energy producers, so it's vital, but the Sun's energy is mostly from making He4 out of D, He3 & T. Easy to overlook, but worth remembering.
 

1. What is proton-proton fusion?

Proton-proton fusion is a type of nuclear reaction in which two protons combine to form a helium nucleus. This process is also known as the proton-proton chain or the pp-chain, and it is the primary source of energy in stars like our Sun.

2. How does proton-proton fusion work?

In proton-proton fusion, two protons fuse together to form a deuterium nucleus. This process releases a positron and a neutrino as byproducts. The deuterium nucleus then fuses with another proton to form a helium-3 nucleus, which then combines with another helium-3 nucleus to form a helium-4 nucleus. This final step releases two protons, which can then continue the cycle.

3. What conditions are necessary for proton-proton fusion to occur?

Proton-proton fusion requires extremely high temperatures and pressures, which are found in the core of stars. These conditions are necessary to overcome the repulsive force between two positively charged protons and allow them to fuse together. In our Sun, the temperature at the core is about 15 million degrees Celsius.

4. Why is understanding proton-proton fusion important?

Proton-proton fusion is the process that powers the Sun and other stars, making it crucial for our understanding of stellar evolution and the universe as a whole. It also plays a role in the production of elements heavier than hydrogen, such as helium and carbon, which are essential for life on Earth. Additionally, scientists are exploring ways to harness proton-proton fusion as a potential source of clean and abundant energy.

5. Are there any challenges in studying proton-proton fusion?

Studying proton-proton fusion is challenging because it occurs at extremely high temperatures and pressures that are difficult to recreate in a laboratory setting. Scientists use computer simulations and data from astronomical observations to understand this phenomenon. Additionally, there are still some uncertainties and gaps in our understanding of the proton-proton fusion process, which scientists are actively researching and trying to unravel.

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