Can iron form via processes like the r- or s-process?

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In summary, iron can form in stars through both silicon burning and beta-decay of neutron-rich isotopes, but these are not the only processes involved in the cosmogenesis of iron. While silicon burning produces a significant amount of iron, it may contribute to Fe-58 and Fe-57. However, the half-life of Mn-56 is only 2.5 hours, so the s-process cannot lead to Fe-57 and Fe-58. Adding neutrons to chromium can also lead to stable isotopes of iron, such as Cr-53, Cr-54, and Cr-55. The alpha process and photodisintegration of Nickel-58 may also result in the formation of iron, while the pair instability supernova
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Teichii492
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Can iron form via processes other than during silicon burning? e.g. the r- or s-process
Hi,

I was wondering by what other methods iron can form in stars? Iron can form during silicon burning and i assume it can also form via the beta- decay of neutron rich isotopes around the iron peak? Are these athe only two processes that relate to the cosmogenesis of iron?
 
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I'm certain there will be the occasional iron atom formed in these processes - but silicon burning produces so much more that it doesn't matter.
It might contribute to Fe-58 (0.3% of natural iron) and Fe-57 (2.1%).

Edit: Mn-56 has a half life of only 2.5 hours, so the s-process won't lead to Fe-57 and Fe-58.
 
  • #3
mfb said:
...Edit: Mn-56 has a half life of only 2.5 hours, so the s-process won't lead to Fe-57 and Fe-58.
Chrome 52 is stable. adding neutrons to cr 53, and then cr54 are still stable. One more gets Cr55 which then beta decays to Mn55 which is stable. One more neutron is Mn 56 which beta decays to Fe56. Then add neutrons to get Fe 57 and Fe 58.

Vanadium 51 is stable. add neutron for V52 which beta decays to Cr52. All isotopes of Ti are stable 46 to 50. and Ti51 decays to V51. Sc46 beta decays to Ti46. Ca 45 decays to Sc 45. You can keep working backwards all the way.
 
  • #4
Is it still the s-process if you start with Fe-56 that has so much more important origins? Eh, whatever.
Surprisingly, Fe56+n -> Fe-57 releases energy.
 
  • #5
Whereas s-process skips Fe-54. How is Fe-54 formed?
Since Fe-59 has half-life 45 days, r-process forms Fe-60... which, however, has half-life 2,6 million years.
 
  • #6
snorkack said:
Whereas s-process skips Fe-54. How is Fe-54 formed?
Since Fe-59 has half-life 45 days, r-process forms Fe-60... which, however, has half-life 2,6 million years.

Alpha process maybe. Ti-46 becomes Cr-50 becomes Fe-54. Photodisintegration of Nickel 58 might get the job done too. Pair instability supernova would have hydrogen present while temperatures are high enough to shove protons in there. So decay of Co-54.

I do not know what happens if you start the alpha process from Oxygen-18 instead of Oxygen-16.
 

1. What is the r-process and how does it contribute to the formation of iron?

The r-process, or rapid neutron capture process, is a nuclear reaction that occurs in supernovae explosions. During this process, heavy elements like iron are formed by the rapid capture of neutrons by existing nuclei. This contributes to the formation of iron because it combines lighter elements with neutrons to create heavier elements, including iron.

2. Can the s-process also contribute to the formation of iron?

Yes, the s-process, or slow neutron capture process, can also contribute to the formation of iron. This process occurs in the cores of stars, where slower neutron capture reactions occur over a longer period of time. The s-process creates elements up to iron by adding neutrons to existing nuclei.

3. How does the formation of iron through these processes affect the overall composition of the universe?

The formation of iron through the r- and s-processes plays a crucial role in the overall composition of the universe. Iron is one of the most abundant elements in the universe, and its formation through these processes helps create the building blocks for planets, stars, and even life.

4. Are there any other processes besides the r- and s-processes that can form iron?

Yes, there are other processes that can contribute to the formation of iron. These include the p-process, or proton capture process, which occurs in the outer layers of stars, and the nu-process, which occurs in supernovae explosions. However, the r- and s-processes are the main contributors to the formation of iron.

5. How do scientists study the formation of iron through these processes?

Scientists study the formation of iron through the r- and s-processes by analyzing the isotopic composition of meteorites, which are remnants of the early solar system. They also use computer simulations and observations of supernovae explosions to better understand how these processes contribute to the formation of iron.

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