Universe
Universe
11th Edition
ISBN: 9781319039448
Author: Robert Geller, Roger Freedman, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 16, Problem 10CC
To determine

The reason for the detection of thrice the number of neutrinos in the experiments conducted by the SNO, as compared to the experiments of the Kamiokande Observatory.

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We saw that, on Earth, the number flux of solar neutrinos from the p-p chain is 6.7E10 s-1 cm-2. Other nuclear reactions in the Sun supplement this neutrino flux with a small additional flux of higher-energy neutrinos. A neutrino detector in Japan, named Super Kamiokande, consists of a tank of 50kton of water, surrounded by photomultiplier tubes. The tubes detect the flash of Cerenkov radiation emitted by a recoiling electron when a high-energy neutrino scatters on it. Calculate the detection rate for neutrino scattering in events per day, if 10-6 of the solar neutrinos have a high enough energy to be detected by this experiment, and each electron poses a scattering cross section=10-43 cm. Hint: Consider the density of neutrino targets "seen" by an individual electron, with a relative velocity of c between the neutrinos and the electron, to obtain the rate at which one electron interacts with the incoming neutrinos, and multiply by the total number of electrons (I've already done this:…
Why was the Davis experiment only able to detect one-third of the neutrinos originally predicted?     Most of the neutrinos were absorbed by Earth’s atmosphere.     The neutrinos combined with other particles as they entered Earth’s atmosphere.     The neutrinos distributed evenly among three different flavors while traveling to Earth.     The number of neutrinos was too great to be held in the tank that Davis designed.     The other two-thirds of neutrinos dissipated while traveling to Earth.
Where did the values for (T - 20 C) come from?
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