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Natural neutrinos

Natural neutrinos. 1. Sun, n e , 60 10 9 /cm 2 /s on earth 2. Atmosphere, 2 n m /1 n e , 100 /m 2 /s 3. Supernova (type II), n m , n e , n t , 10 58 in 10 s. Cerenkov effect. When a charged particle propagates at a velocity > c/n Water n=1.33 V=220000km/s EM shock wave

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Natural neutrinos

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  1. Natural neutrinos 1. Sun, ne, 60 109 /cm2/s on earth 2. Atmosphere, 2nm/1ne, 100 /m2/s 3. Supernova (type II), nm, ne, nt, 1058 in 10 s

  2. Cerenkov effect When a charged particle propagates at a velocity > c/n Water n=1.33 V=220000km/s EM shock wave Light emission over a cone cos q = 1 / bn

  3. The SuperKamiokande detector • Built under a mountain in Japan, SuperK is an immense reservoir of 50 kilotons of purified water, seen by 11000 giant phototubes. • ne from the Sun interact on electrons. • Cerenkov effect for energies above 5 MeV.

  4. Neutrinos from SN1987 Kamiokande 1000 tons of water Looking for… proton decay 23 february 1987

  5. Standard solar model

  6. Solar neutrinos • Main fusion reaction • 4p 4He + 2e+ + 2ne + 27 MeV. • Knowing the solar luminosity, this gives a flux of 60 106/cm2/s arriving on earth surface. • Neutrinos from the main chain have an energy limited to 430 keV, but other secondary production processes give neutrinos up to 15 MeV.

  7. Solar neutrino spectrum

  8. Detection with SuperK • In 1500 days, SuperK • detected 22000 events • while 48000 were predicted. • This is the so-called deficit • of solar neutrinos • Already seen with Homestake and Gallex/Sage experiments.

  9. Prehistory of solar neutrino searches Radiochemical searches 1. Homestake chlorine experiment 615 tons of tetrachloroethylene n + 37Cl37Ar + e- 2. Gallex/Sage 15 tons of watered gallium 71 n + 71Ga71Ge + e-

  10. Homestake

  11. Gallex

  12. Solar neutrino results • Homestake deficit • Seen/expected = 0.3 • Gallium deficit • Seen/expected = 0.6 • SuperK deficit • Seen/expected = 0.45 • The deficit changes with energy!

  13. Atmospheric neutrinos • New deficit observed. • Production 2 nm pour 1 ne from all horizons. A few 100 MeV energy. • SuperK distinguishes e and m • Azimuthal distribution of ne OK • But for nm deficit for neutrinos crossing the earth, having propagated over few 1000 km.

  14. Do neutrinos oscillate? • The deficits can be explained by a change of flavor during propagation

  15. Case of two neutrino flavors Old idea from B. Pontecorvo: same as in K0 system Weak interaction eigenstates ne, nm different from mass eigenstates (propagation) n1, n2 Mixing matrix unitary 2x2 • ne = n1 cosq + n2 sinq • nm = -n1 sinq + n2 cosq • Probability of oscillation • P = sin22q sin2(pR/L) • with L = 2,5 E(GeV)/Dm2(eV2)  Two unknows Dm2 and sin22q

  16. Experimental hints 1. Deficit of solar neutrinos Disappearance of ne 2. Deficit of atmospheric neutrinos Diappearance of nm Note: experimentally 2 complementary search methods, disappearance of initial neutrinos or appearance of new flavor not present at the source

  17. SK result (atmospheric nm)

  18. Pontecorvo-Maki-Nakagawa-Sakata matrix Three neutrinos. Mixing matrix, unitary 3x3 3 mixing angles + 1 phase Solar neutrinos q12, Dm122 Atmospheric neutrinos q23, Dm232 Remains to measure: q12, d and absolute mass scale

  19. Resonant oscillation in matterMSW effect MSW effect can produce an energy spectrum distortion and flavor regeneration in Earth giving a Day-night effect. In fact, for solar n, oscillations occur inside the Sun. When observed, matter interactions define the mass hierarchy

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