Solar Neutrino and Neutrino Physics in Brazil
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1 Solar Neutrino and Neutrino Physics in Brazil Pedro Cunha de Holanda DRCC - IFGW UNICAMP Florence, 2012
2 A little bit of history
3 A little bit of history my
4 A little bit of history Pontecorvo: Solar Neutrinos, maybe we can detect them, maybe the flux will agree with solar model predictions, and if they don't agree, maybe the neutrinos are oscillating. Davis: First solar neutrino detection at Homestake. Ok, but oscillation is not a good mechanism, because it only works for large mixing angles.
5 A little bit of history Pontecorvo: Solar Neutrinos, maybe we can detect them, maybe the flux will agree with solar model predictions, and if they don't agree, maybe the neutrinos are oscillating. Davis: First solar neutrino detection at Homestake. Ok, but oscillation is not a good mechanism, because it only works for large mixing angles. But there are matter effects!
6 A little bit of history Pontecorvo: Solar Neutrinos, maybe we can detect them, maybe the flux will agree with solar model predictions, and if they don't agree, maybe the neutrinos are oscillating. Davis: First solar neutrino detection at Homestake. Ok, but oscillation is not a good mechanism, because it only works for large mixing angles. But there are matter effects! No good, matter effects are diagonal in evolution matrix, and then decrease oscillation signal.
7 A little bit of history Pontecorvo: Solar Neutrinos, maybe we can detect them, maybe the flux will agree with solar model predictions, and if they don't agree, maybe the neutrinos are oscillating. Davis: First solar neutrino detection at Homestake. Ok, but oscillation is not a good mechanism, because it only works for large mixing angles. But there are matter effects! No good, matter effects are diagonal in evolution matrix, and then decrease oscillation signal. MSW mechanism enhance conversion even for very small mixing angles!
8 A little bit of history Year: 1998 Data: - Homestake, total rate - Gallex and Sage, total rate - Super-Kamiokande I (504 days), rates, day-night assymetry, spectrum. Solutions: - SMA - oscillation in vacuum Bahcall, Krastev and Smirnov, Phys.Rev.D58(1998)
9 A little bit of history Year: 1999 Data: - Homestake, total rate - Gallex and Sage, total rate - Super-Kamiokande I (708 days), rates, day-night assymetry, spectrum information. Solutions: - LMA? Bahcall, Krastev and Smirnov, Phys.Rev.D60(1999)
10 A little bit of history Year: 2000 Data: - Homestake, total rate - Gallex and Sage, total rate - Super-Kamiokande I (825 days), rates, zenith angle distribution, spectrum and seasonal variation. Solutions: - SMA, LOW, LMA - oscillation in vacuum - RSFP - NSNI - VEP M. C. Gonzalez-Garcia, PCH, C. Peña-Garay and J.W.F. Valle Nucl.Phys.B573(2000), 3-26.
11 A little bit of history Year: 2002 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. - SNO, charged current Solutions: A.M. Gago, M.M. Guzzo, PCH, H. Nunokawa, O.L.G. Peres, V. Pleitez, R. Zukanovich Funchal, Phys.Rev.D65 (2001), LOW, LMA - oscillation in vacuum - RSFP - NSNI - VEP
12 A little bit of history Year: 2002 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. - SNO, charged current Solutions: A.M. Gago, M.M. Guzzo, PCH, H. Nunokawa, O.L.G. Peres, V. Pleitez, R. Zukanovich Funchal, Phys.Rev.D65 (2001), LOW, LMA - oscillation in vacuum - RSFP - NSNI - VEP
13 A little bit of history Year: 2002 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. - SNO, charged current Solutions: - LOW, LMA - oscillation in vacuum - RSFP - NSNI - VEP
14 A little bit of history Year: 2003 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. - SNO, charged current day-night spectrum - KamLAND, spectrum Solutions: PCH, A. Yu. Smirnov, JCAP 02 (2003) LMA
15 A little bit of history Year: 2003 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. Linear scale! - SNO, charged current day-night spectrum - KamLAND, spectrum Solutions: PCH, A. Yu. Smirnov, JCAP 02 (2003) LMA
16 A little bit of history Year: 2004 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. Linear scale! - SNO, charged current day-night spectrum, NC and ES rates. - KamLAND, spectrum Solutions: PCH, A. Yu. Smirnov, Astropart.Phys.21 (2004) LMA
17 A little bit of history Year: 2011 Data: - Homestake, total rate - Gallex, GNO and Sage, total rate - Super-Kamiokande, rates, zenith angle distribution, spectrum and seasonal variation. - SNO, CC, NC and ES day-night spectrum, all fases - Borexino. - KamLAND, spectrum G.A.Valdiviesso, M.M. Guzzo, PCH, Phys.Lett. B (2011) 240. Solutions: - LMA
18 MSW-LMA: robust solution
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24 Solar neutrino experiments - latest data -
25 Super-Kamiokande IV Smy, Neutrino 2012
26 Super-Kamiokande IV Smy, Neutrino 2012
27 Super-Kamiokande IV Smy, Neutrino 2012
28 Sudbury Neutrino Observatory, I & II SNO Collaboration, Phys.Rev.C81:055504,2010
29 Sudbury Neutrino Observatory, I & II SNO Collaboration, Phys.Rev.C81:055504,2010
30 Sudbury Neutrino Observatory, I & II Test of spectral distortion following a SNO prescription through expansion of survival probability: and correlations between coeficients: SNO Collaboration, ArXiV:
31 Sudbury Neutrino Observatory, I & II McDonald talk, Neutrino 2012
32 8 Borexino, measurement of B flux
33 Borexino PLUS: Measurement of 7Be neutrino flux, and absence of day-night variation (exluding LOW solution and a particular exotic scenario) Borexino Coll. Phys.Rev.Lett.107(20011) Measurement of pep neutrinos. PCH, JCAP07(2009)024
34 Putting everything together Smy talk, Neutrino 2012 McDonald talk, Neutrino 2012
35 New physics related to tension between solar and KamLAND prefered mass scale
36 New physics related to tension between solar and KamLAND prefered mass scale You're are not suppose to name it. Once you name it, you start getting attached to it!
37 New physics related to tension between solar and KamLAND prefered mass scale - 4th (sterile) neutrino with low mass. PCH and A. Yu. Smirnov, Phys.Rev.D83 (2001) MaVaN's, NSNI, magnetic moment...
38 Smirnov and Brazil
39 Smirnov and Brazil
40 Smirnov and Brazil Quite a strong group of people talking about neutrino physics. From this group, Alexei Smirnov collaborated with Orlando Peres (Unicamp), myself (Unicamp) and Renata Zukanovich Funchal (USP). To put some numbers, in 15 years we can count from direct collaboration with Alexei Smirnov, 14 papers on neutrino phenomenology, involving solar, atmospheric, and reactor neutrinos. And hopefully, the collaboration continues!
41 Smirnov and Brazil Quite a strong group of people talking about neutrino physics. From this group, Alexei Smirnov collaborated with Orlando Peres (Unicamp), myself (Unicamp) and Renata Zukanovich Funchal (USP). To put some numbers, in 15 years we can count from direct collaboration with Alexei Smirnov, 14 papers on neutrino phenomenology, involving solar, atmospheric, and reactor neutrinos. And hopefully, the collaboration continues! Thank you, Alexei!
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KamLAND Data and the Solution to the Solar Neutrino Problem
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