Calculating Neutrino Energy in PPI Chain

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SUMMARY

The discussion focuses on calculating the percentage of energy carried away by neutrinos in the proton-proton (PPI) chain. It emphasizes the need for standard kinematics to determine the energy spectrum of neutrinos, which arises from a three-body reaction. Key techniques involve applying energy and momentum conservation principles, along with comparing results to the solar neutrino energy spectrum illustrated in Figure 2 of Bahcall, Serenelli, and Basu (2005). The complexity of calculating neutrino fluxes is also noted, indicating a significant increase in difficulty.

PREREQUISITES
  • Understanding of proton-proton (PPI) chain reactions
  • Familiarity with kinematics and energy conservation principles
  • Knowledge of neutrino physics and energy spectra
  • Access to Bahcall, Serenelli, Basu (2005) for reference
NEXT STEPS
  • Study the energy spectrum of solar neutrinos as presented in Bahcall, Serenelli, Basu (2005)
  • Explore advanced kinematic calculations in three-body reactions
  • Research methods for calculating neutrino fluxes in astrophysical contexts
  • Investigate the implications of neutrino energy loss in stellar processes
USEFUL FOR

Astronomers, physicists, and students interested in nuclear astrophysics, particularly those studying solar neutrinos and energy transfer in stellar processes.

Billg4444
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How would i go about working out the percentage of energy carried away by neutrinos in a PPI chain?
 
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Thanks for the post! Sorry you aren't generating responses at the moment. Do you have any further information, come to any new conclusions or is it possible to reword the post?
 
So, out of PPI, you'll find that the neutrinos will have a spectrum of energies, since their production is a three body reaction. You'll just need to do some pretty standard kinematics to find out what that spectrum should be - you know the masses of the entrance and exit channel, and you can find a range of appropriate kinetic energies for the entrance channel. The rest is energy/momentum conservation.

You can compare your results to Fig. 2 of Bahchall, Serenelli, Basu (2005), which shows the solar neutrino energy spectrum for a pretty good solar model. Calculating the fluxes of those neutrinos is another few orders of magnitude in difficulty. ;)
 

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