'Solar neutrino experiments' diaporamas de présentation

Neutrinos at the forefront of elementary particle physics and astrophysics October 22, 2012

Neutrinos at the forefront of elementary particle physics and astrophysics October 22, 2012. Neutrinos at the forefront of elementary particle physics and astrophysics, October 22, 2012. Searches for sterile neutrinos. Michel Cribier CEA/DSM Irfu/SPP & APC-Paris. Need ?.

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Solar Neutrinos, Neutrino Cross Sections, and NUSEL Developments

Solar Neutrinos, Neutrino Cross Sections, and NUSEL Developments. A.B. Balantekin ORNL SNS Workshop August 28, 2003. Puzzles where neutrinos may play a role. What is the Dark Matter made of? What is Dark Energy? How much neutrinos contribute and why? (what is ? ? ?)

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Neutrinos as Probes: Solar-, Geo-, Supernova neutrinos; Laguna

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Neutrinos as Probes: Solar-, Geo-, Supernova neutrinos; Laguna

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What Are Neutrinos Anyway and What Is All This Fuss About?

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Status and future prospects of Gran Sasso

Status and future prospects of Gran Sasso. Aldo Ianni INFN Gran Sasso Laboratory NNN05 Aussois, April 7-9. The Gran Sasso Underground Laboratory. Proposed in 1979 Approved in 1982 Since 1989 w/ the first experiment: MACRO. Scientific achievements. Neutrino oscillations:

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The Elementary Particles

The Elementary Particles. The Basic Interactions of Particles. e ?. u. d. ?. ?. ?. e ?. u. d. u, d. d. e ?. g. W +. W +. u, d. u. ? e. e ?. ?. u, d. Z 0. Z 0. Z 0. e ?. ?. u, d. Weak Nuclear Force . Electromagnetic Force. Charged Current . Strong Nuclear Force .

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Neutrino emission

Neutrino emission. <E>=0.27 MeV. E=0.39,0.86 MeV. <E>=6.74 MeV. ppIII loss: 28%. ppII loss: 4%. ppI loss: ~2%. note: <E>/Q= 0.27/26.73 = 1%. Total loss: 2.3%. 2 neutrino energies from 7Be electron capture ?. 7 Be + e - ? 7 Li + n e. E n. E n. Continuous fluxes in /cm 2 /s/MeV

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Writing: Friend or Foe?

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solar neutrino physics

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