Why is the zenith angle distribution of the muons cos2(x) ?

In summary, the flux distribution of cosmic ray muons follows a cos^2(θ) pattern, which is considered an experimental fact without a clear explanation. This is because the Earth's atmosphere is a spherical shape and the path length for θ=0 is the minimum possible, making it more likely to detect muons at smaller angles. The Bethe-Bloch formula also supports this distribution, as well as the fact that the Earth's atmosphere is not a perfect sphere. This distribution has been proven through experimental data and is considered an approximation without a way to derive it. If cosmic rays were uniform and isotropic, a distribution of 1/cos(θ) would be expected, but the presence of the Earth's atmosphere makes
  • #1
phys_student1
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Hello,

Empirically, the flux distribution of cosmic ray muons follow cos^2(θ) where θ is angle of incidence. Looking up the papers, I did not find any clue as to why is this the case. All sources simply consider this an experimental fact.

Is their any real explanation for this?
 
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  • #2
That is a common question and I never saw a good answer. It is probably just some function which is not so far away from the real distribution, without a deeper physical argument behind it.
 
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  • #3
First of all consider that the Earth's atmosphere is a perfect sphere.
The path length for θ=0 is the minimum possible.
Also note that there no chance to detect a muon for θ=π/2(for this specific angle the muon would have to travel along the Earth's crust, it would collide and interact with the crust's atoms with a very high probability).

Those arguments state that we need a cos-like distribution.

The next step is to think that the muon obeys the Bethe-Bloch formula. In simple words the energy loss per unit length, is something like 1/β^2...

This implies that it is very much likely to observe a muon for small θ(where the path length is minimum) rather that large θ, in a non-linear way.

If you also put in mind that the Earth's atmosphere isn't a perfect sphere, but it's a "3D ellipsoidal", you are again moving away from linearity.

I believe that Andersson has done some "fitting" on experimental data of cosmic ray flux, which proves the cos^2θ distribution.

So it is an experimental model, as far as I know.
 
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  • #4
This is an approximation, and as such, you won't be able to derive it.

If cosmic rays were uniform and isotropic, you'd expect a distribution that goes more like 1/cos(theta), because there's not a lot of area with a small zenith angle compared to a large one. However, as atha points out, we have an atmosphere, so cosmic rays from the horizon are unlikely to make it to us.
 
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  • #5
Thanks all. Yes I also looked too much in the literature without finding any clue, all state is as empirical formula or experimental fact. Thanks for your responses.
 

1. Why is the zenith angle distribution of muons described by cos2(x)?

The zenith angle distribution of muons follows a cos2(x) pattern because muons are produced from the decay of pions in the upper atmosphere, which have a preferred direction of travel. As muons travel through the atmosphere, they experience less and less interaction with air molecules, resulting in a larger proportion of muons arriving at the Earth's surface at lower angles. This results in a cosine distribution, with an additional squared term due to the relativistic effects of time dilation and length contraction.

2. How does the Earth's magnetic field affect the zenith angle distribution of muons?

The Earth's magnetic field can deflect charged particles, including muons, as they travel through the atmosphere. This can result in a slight distortion of the expected cos2(x) distribution, as muons may be deflected towards the poles, resulting in a higher concentration of muons at higher zenith angles near the equator and a lower concentration near the poles.

3. Does the zenith angle distribution of muons change depending on the altitude?

Yes, the zenith angle distribution of muons can vary at different altitudes. This is due to the fact that the atmosphere becomes less dense at higher altitudes, resulting in less interaction and deflection of muons. This can result in a slightly flatter distribution at higher altitudes compared to near the Earth's surface.

4. Can the zenith angle distribution of muons be used to study the properties of the atmosphere?

Yes, the zenith angle distribution of muons can provide valuable information about the composition and density of the atmosphere. By measuring the deviation from the expected cos2(x) distribution, scientists can infer the presence of different atmospheric layers and their properties, such as the ozone layer and the density of air molecules at different altitudes.

5. How can the zenith angle distribution of muons be measured?

The zenith angle distribution of muons can be measured using various types of detectors, such as scintillators or Cherenkov detectors. These detectors can be placed at different altitudes or angles to measure the flux of muons arriving at different angles. By analyzing the data collected from these detectors, scientists can determine the zenith angle distribution of muons and study its properties.

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