Gzk paradox and expanding universe

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SUMMARY

The discussion centers on the GZK paradox and its relation to cosmic rays and supernovae. Participants explore the implications of a hypothetical universe divided into two mass zones, which could explain why high-energy cosmic rays, expected to be stopped by the cosmic microwave background radiation (CMBR), still reach Earth. Key calculations indicate that cosmic ray protons with energies greater than 50 EeV should only travel less than 100 million light-years before colliding with CMBR photons. The conversation highlights the role of relativistic effects on quark size and collision probabilities, referencing Stecker's work on the GZK effect.

PREREQUISITES
  • Understanding of the GZK effect and its implications for cosmic rays
  • Familiarity with cosmic microwave background radiation (CMBR) and its density
  • Knowledge of special relativity and its effects on particle physics
  • Basic concepts of supernovae and their role in cosmic expansion
NEXT STEPS
  • Study the GZK effect in detail, particularly Stecker's discussions in relevant literature
  • Research cosmic microwave background radiation (CMBR) and its impact on high-energy cosmic rays
  • Explore the implications of relativistic length contraction on particle interactions
  • Investigate the behavior of high-energy protons in air showers and their collision dynamics
USEFUL FOR

Astronomers, physicists, and researchers in high-energy particle physics, particularly those focused on cosmic ray studies and the implications of the GZK paradox.

kurious
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If the universe were divided into two mass zones, and one zone
repelled the other,supernovae would not only accelerate away from us
but the zone in which we are living would accelerate away from the
supernovae.Also cosmic rays could be repelled by one zone and pushed
through another.Could this explain the GZK paradox where highly
energetic cosmic rays that should have been stopped from reaching the
Earth by the microwave background have not been stopped?
 
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I'm not sure I understand what you're saying here; perhaps a few numbers might help.

First, re supernovae 'accelerating away from us': the 'high-z' supernovae (SN) which provide evidence for the 'acceleration' are ~5 to 10 billion light years away (well, more accurately, the light which we now see from them has traveled for 5 to 10 billion years to get to us). Closer SN do not really show a deviation from the Hubble expansion rate (~71 km/s/Mpc), though the 'acceleration' surely affects what we see of them too (there are also plenty of SN which seem to be further, or closer, to us than the Hubble relation would suggest; however, these deviations are well understood as the result of the motion of the host galaxies in the gravitational field of the cluster - or super-cluster - in which they reside).

Then the GZK limit: based on the density of CMBR photons (~400 per cubic centimetre), cosmic ray protons with an energy of ~>50 EeV (1 EeV = 1018 eV) should only be able to travel ~<100 Mly before they collide with a CMBR photon and produce lots of pions.

You can see that these distances are quite different, so it's hard to see how the acceleration of distant SN and the GZK limit they would be connected.
 
see reply below
 
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You can see that these distances are quite different, so it's hard to see how the acceleration of distant SN and the GZK limit they would be connected

I agree with what you have said. Suppose the quarks in cosmic ray protons have a size i.e
if they consisted of spheres of charge, and by special relativity length contraction these spheres got small at high speeds and energies, this would reduce the probability of a collision with a CMBR photon and allow the proton to reach the Earth.
 
Stecker has a good discussion of the GZK effect (see Section 2.2, starting on p7). It also contains references to the original papers by Griesen, Zatsepin, and Kuz'min, as well as several others on the topic.

I think you will find that relativity effects were taken into account in making the calculations, particulary wrt the "energy dependence of the photomeson production cross sections and inelasticities", i.e. how likely it is that a proton of energy x will collide with a CMBR photon, for different kinds of collision.
 
Thanks for the reference.It's full of useful reading.
think you will find that relativity effects were taken into account in making the calculations, particulary wrt the "energy dependence of the photomeson production cross sections and inelasticities", i.e. how likely it is that a proton of energy x will collide with a CMBR photon, for different kinds of collision.



I've done a calculation that shows that a sphere of charge in a quark is 10^-18 m when the quark has no speed.This is one thousand times smaller than a proton at rest.So relativistic length contraction would make the quark even smaller and less likely to interact with the CMBR than expected using the normal proton size.
 
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kurious said:
I've done a calculation that shows that a sphere of charge in a quark is 10^-18 m when the quark has no speed.This is one thousand times smaller than a proton at rest.So relativistic length contraction would make the quark even smaller and less likely to interact with the CMBR than expected using the normal proton size.
The same considerations would surely also need to have been made re high energy protons colliding with particles such as oxygen nuclei, leading to different behaviour for air showers (for example) than what has been observed. The same effects would also occur - at much lower energies - in the LHC and its predecessors.

There's certainly some interesting physics in the >100 GeV regime, such as the formation of a new state of matter, http://www.bnl.gov/rhic/QGP.htm, but AFAIK studies of these phenomena haven't lead to big changes in estimates of collision cross-sections.
 
gzk paradox

The same considerations would surely also need to have been made re high energy protons colliding with particles such as oxygen nuclei, leading to different behaviour for air showers (for example) than what has been observed. The same effects would also occur - at much lower energies - in the LHC and its predecessors.

But the size of the quarks only determines the chance of a collision - not the outcome of the collision - assuming the number of oxygen quarks is similar to the number of microwaves a cosmic ray proton encounters on its journey.
 
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