Cross section-temperature equivalence

In summary, the interaction rate between two particles, m and l, is expressed as Γm=<nlσv>, where nl is the density of species l, σ is the cross-section of species m, and v is the relative velocity between the two particles. It is also assumed that <σv>∼G²T², where G is fermi's constant. It is unclear where this assumption comes from and it may not be true in general, as it is based on the assumption of weak interaction in GF.
  • #1
karmion
1
0
It's assumed that interaction rate between a species of particule m and l is expressed as:

Γm=<nlσv>,

where nl is the density of the species l, σ the cross-section of species m (=probability of interaction) and v the relative velocity between the two particles.

It's also assumed that <σv>∼G²T², where G is fermi's constant.

I need to know where comes from this last equivalence relation, is there anyone that can help me please ?
 
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  • #2
I don't know where this came from, but it is not true in general, as GF assumes a weak interaction, That's not true for particles in general.
 
  • #3
karmion said:
It's assumed that ...
Where is it assumed?
 

FAQ: Cross section-temperature equivalence

What is cross section-temperature equivalence?

Cross section-temperature equivalence refers to the relationship between the effective cross-sectional area of particles and the temperature of the system in which they are present. This concept is often used in fields like nuclear physics and astrophysics to describe how interactions between particles change with temperature.

How is cross section-temperature equivalence used in nuclear physics?

In nuclear physics, cross section-temperature equivalence is used to predict the behavior of particles during nuclear reactions. As temperature increases, particles move faster and the likelihood of interactions (captured by the cross-sectional area) changes. This relationship helps in modeling nuclear reactions and understanding reactor behavior.

Why is understanding cross section-temperature equivalence important in astrophysics?

In astrophysics, understanding cross section-temperature equivalence is crucial for modeling stellar environments and cosmic phenomena. It helps in predicting the rates of nuclear fusion reactions in stars, the behavior of particles in supernovae, and the formation of various elements in the universe.

How does temperature affect the cross-sectional area of particles?

As temperature increases, particles gain kinetic energy and move more rapidly. This increased movement can lead to a higher probability of interactions, effectively increasing the cross-sectional area. Conversely, at lower temperatures, particles move more slowly, leading to fewer interactions and a smaller effective cross-sectional area.

Can cross section-temperature equivalence be applied to non-nuclear systems?

Yes, the concept of cross section-temperature equivalence can be applied to non-nuclear systems, such as chemical reactions and material science. In these fields, understanding how temperature affects interaction probabilities can help in designing better materials and optimizing chemical processes.

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