f10_oct28 - The Hunt for Solar Neutrinos II. - Kamiokande...

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Used a large tank of H 2 O water (initially 3,000 gallons) to detect ! -e - collisions via light flashes (Cerenkov radiation) seen by photomultiplier tubes Kamioka mine in Japan The Hunt for Solar Neutrinos II. - Kamiokande (the original) Solar ! ‘s: SuperKamiokande An accident in 2001 blew out most of the sensors; they were repaired, operations resumed in 2003 Which Neutrinos Could they See? Both the Davis and Kamiokande experiments could detect only high-energy neutrinos; they could not see the neutrinos produced in the first step of the p-p chain (which makes deuterium), but only some rare ones made by variations of the third step (which makes helium-4)
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Neutrinos Produced by H Fusion Chasing the Low-Energy Neutrinos: The Gallium Experiments The Solar Neutrino Spectrum The Solar Neutrino Problem TOO FEW SOLAR NEUTRINOS DETECTED, COMPARED TO PREDICTIONS FROM MODELS
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The Solution: Neutrino Oscillations Solar fusion reactions create only one type of neutrinos, “electron neutrinos” but two other kinds (muon, tau) exist • Some people theorized that some of the neutrinos were changing into other kinds en route from the Sun’s core • The Davis experiment could see only electron neutrinos • Kamiokande was used to detect a beam of neutrinos coming from 250 km away (“Kam-LAND”), proving that the neutrinos were changing types Sudbury Neutrino Observatory (SNO) Solar ! observatory in
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This note was uploaded on 04/30/2011 for the course AST 317 taught by Professor Dinerstein during the Fall '10 term at University of Texas.

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f10_oct28 - The Hunt for Solar Neutrinos II. - Kamiokande...

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