Solar Neutrinos. Neutrino light from the Sun (Super-Kamiokande) energy of the neutrinos in MeV

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1 Solar Neutrinos 4 p He 4 + 2e ν e MeV Neutrino light from the Sun (Super-Kamiokande) energy of the neutrinos in MeV

2 Solar Neutrinos: pioneering experiment Nobelprize 2002 Since 1970 ν e Cl Ar + e E ν > 814 kev R exp = 0.34 SSM Raymond Davis Jr., Homestake Experiment

4 Ar Counting: Ar + e ν e + Cl T 1/2 = 35 Tage

5 SSM

6 Gran Sasso Untergrundlabor (Italien) 150 km von Rom Teramo Autostrada Rom

7 ve Ga Ge + e - E v > 233 kev

8 Extraction of 71 Ge (as GeCl 4 ) in GALLEX

9 Conversin to GeH 4

10 e Ge Ga + T 1/2 = 11.4 d v e

11 Result: /- +/-8 SNU SSM prediction: /-6 SNU (BP98) expected without oscillation

12 SAGE (soviet american gallium experiment) Heute: BNO (Baksan Neutrino Observatory) Elbrus 5642m Baksan Valley, Kabardino-Balkaria, Russia

14 Messperioden SAGE: SAGE I Jan May 92 Rise time from ADP SAGE II.1 Sep Oct. 93 SAGE II.2 Nov June 94 SAGE II.3 July 94 - Dec. 94 SAGE III.1 Jan June 95 SAGE III.2 July 95 - present Rise time from wave form, begin to use L peak Ga theft period Before Cr experiment Some extractions during Cr experiment After Cr experiment

15 The extraction and concentration of germanium (SAGE): 1. Ge is extracted from the Ga metal into an aqueous solution by an oxidation reaction. 2. The aqueous solution is concentrated. (a) Vacuum evaporation reduces the volume of aqueous solution by a factor of 8. (b) Ge is swept from this solution as volatile GeCl4 by a gas flow and trapped in 1 l of deionized water. (c) A solvent extraction is made from the water which concentrates the Ge into a volume of 100 ml. 3. The gas GeH4 is synthesized, purified, and put into a proportional counter. Mehr unter arxiv:astro-ph/ v2 11 Nov 1999 Phys. Rev. C 60, (1999)

(b) Ge is swept from this solution as volatile GeCl4 by a gas flow and trapped in 1 l of deionized water.

16 Abbildung der Sonne im Neutrinolicht (Super-Kamiokande)

17 Detection of solar neutrinos in Super-Kamiokande: Elastic neutrino electron scattering s v + e vx + e x (dominated by v e ) (Kinematics like Compton effect) ν e,µ,τ ν e,µ,τ t v e can interact via CC + NC v μ and v τ can only interact via NC!

v e ) (Kinematics like Compton effect) ν e,µ,τ ν e,µ,τ t v e

19 First generation of experiments Homestake 37 Cl Gallex 71 Ga SAGE 71 Ga Kamiokande + SuperK H 2 O Cerenkov Raymond Davis Jr. dissapearance of v e! solar neutrino puzzle Masatoshi Koshiba

20 The Solar Neutrino Puzzle Data/SSM(BP98) Energy dependent deficit Kamiokande Gallex Sage Homestake SK 233 kev 814 kev 6.5 MeV Energy Threshold (MeV)

21 View inside the Sun: Helioseismology Measure propagation of sound waves inside the Sun (like seismic waves in the Earth) 3 Types: acoustic, gravity, surface gravity waves -> resonant modes: p modes, g modes, f modes P-mode: Standing waves of the Sun's vibrations: Radial order n = 14, angular degree l = 20, angular order is m = 16. Red and blue show element displacements of opposite sign. The frequency of this mode determined from the MDI data is /- 0.2 microhz.

22 Speed of sound in the Sun radial and latitudinal variations of the sound speed in the Sun, relative to a standard solar model. Red color = positive variations (`hotter' regions), blue color = negative variations (`cooler' regions).

23 The Solar Neutrino Puzzle Data/SSM(BP98) Energy dependent deficit Kamiokande Gallex Sage Homestake SK Helioseismology confirms solar models 233 kev 814 kev 6.5 MeV Non-standard Energy neutrino Threshold properties! (MeV)

24 Status of solar neutrino oscillation spring 2000 LMA SMA LOW VAC tan 2 θ 10

25 Creighton Mine (Nickel) Sudbury, Canada Depth 2070m 1000t D 2 O 9500 PMTs

26 INCO mining co. Viele interessante Erze wg. Meteoriteneinschlag!

28 Neutrino detection in SNO CC ES NC v e v + d p + p + e e + e v e + e v + d p + n + x v x γ

29 Neutrino - Electron Scattering Event

30 Neutron detction in SNO

31 SNO Result (salt-phase) (PRL 92, , 2004)

32 SNO Result (salt-phase) (PRL 92, , 2004) 1/3 der v e kommen auf der Erde an. 2/3 der v e kommen als v µ oder v τ an. Gemessener Gesamtneutrinofluss = SSM Ergebnis Ergebnis der der ersten ersten Phase Phase (one (one Salz): Salz): "Direct "Direct Evidence Evidence for for Neutrino Neutrino Flavor Flavor Tranformation Tranformation from from Neutral-Current Neutral-Current Interactions Interactions in in the the Sudbury Sudbury Neutrino Neutrino Observatory, Observatory, The The SNO SNO Collaboration Collaboration Phys. Phys. Rev. Rev. Lett. Lett. volume volume 89, 89, No. No. 1, 1, (2002). (2002).

34 Oscillation analysis of all solar neutrino experiments LMA SMA LOW VAC tan 2 θ 0 0.4

Solar neutrinos: from their production to their detection

Solar neutrinos: from their production to their detection : from their production to their detection Universitï degli Studi di Milano and Istituto Nazionale di Fisica Nucleare E-mail: Lino.Miramonti@mi.infn.it Nuclear fusion reactions take place in the core of