Neutrinos (reliques) de supernovae et leurs propriétés Cristina VOLPE (Institut de Physique Nucléaire Orsay, FRANCE)

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1 Neutrinos (reliques) de supernovae et leurs propriétés Cristina VOLPE (Institut de Physique Nucléaire Orsay, FRANCE)

2 Physique nucléaire processus double-beta, interaction -noyau,… Physique du neutrino Cosmologie BBN, LSS, leptogènese,… UN DOMAINE AUX NOMBREUSES INTERFACES soleil, SNII, UHE, Astrophysique

3 PLAN II. Neutrinos de supernovae et physique des neutrinos Conclusions et Pespectives I. Neutrinos de supernovae : présent et futur

4 I.THE first OBSERVATION of SOLAR e From fusion reactions, like p+p  2 H+e + + e 1970 the detector Homestake mine (South Dakota) 600 tons of C 2 Cl 4 e + 37 Cl 37 Ar + e - « We observe much less neutrinos than we expect. » « THE SOLAR NEUTRINO PUZZLE » THE IMPORTANT DISCOVERY OF NEUTRINO OSCILLATIONS.

5 THE  CP violating PHASE INTRODUCES A - ASYMMETRY. L  3  e  1  12  23  13 1  3 e   The two basis are related by a unitary matrix, called the Maki-Nakagawa-Sakata- Pontecorvo (MNSP) matrix, which is the analog of the Cabibbo-Kobayashi- Maskawa (CKM) matrix for quarks.  23  13  12 THE OSCILLATION PARAMETERS

6 Totani et al., Astr.. J. 1998 t (s) 0.11. 10 Type II SUPERNOVAE… collapse e burst cooling SN1987AEVENTSSN1987AEVENTS NEUTRINOS FOLLOW CLOSELY THE EXPLOSION MECHANISM. R. Davis and M. Koshiba, 2002 Nobel Prize with R. Giacconi

7 Neutrino Astronomy « To use stars and the Universe for the study of fundamental properties. » The philosophy… Neutrinos mass hierarchy ? the mixing angle  13 ? Majorana or Dirac ? the magnetic moment ? … Type II Supernovae neutrino propagation in the star luminosities, spectra, time distribution of the emitted neutrinos nucleosynthesis (r-process) …

8 FUTURE EXPERIMENTS IMPORTANT DISCOVERY FOR SUPERNOVA AND NEUTRINO PHYSICS. I.To measure the neutrino luminosity curve from a future (extra)galactic explosion. SK 9000 MEMPHYS 140000 EVENTS II. To measure the relic neutrino background from past supernova explosions. Theoretical predictions close to the present experimental limit (1.2 anti- e /cm2/s from Super-Kamiokande). New observatories of large (megaton) size are under study (water Cherenkov, scintillator, liquid argon technologies are considered). A demand for a design study (LAGUNA) submitted within FP7. Such observatories can observe far explosion (much more frequent) and reach the sensitivity to observe relic neutrinos.

9 The possible existence of CP violation in the lepton sector is a crucial issue that will be addressed by « third generation » experiments (super-beams, beta-beams, neutrino factories). Can we use supernova neutrinos to learn about CP violation in the lepton sector ? Thèse de Jérome Gava

10 A.B. Balantekin, J. Gava, C. Volpe, arXiv:0710.3112 CP VIOLATION AND SUPERNOVA  e  (  =180 o )  e (  =0 o )    (  =180 o )   (  =0 o ) Numerically, we have solved the evolution with a non-zero phase : Analytically, we have demonstrated that : - if the  and  fluxes are equal at emission, there is no CP effect on the (anti)- e fluxes. SIGNIFICANT CP EFFECTS. effects in an observatory? - if the  and  fluxes differ at emission (ex. physics beyond the Standard Model), there are significant effects from the  phase on the (anti)- e fluxes.

11 e + p n + e+ e atmospheric background relic e flux hierarchy  13 e reactor background RELIC SUPERNOVA Relic neutrino fluxes bring information about the explosion, the supernova formation rate and neutrino properties. C. Volpe, J. Welzel, arXiv:0711.3237 We have performed a detailed analysis of the three technologies considered for future observatories and proposed to measure both electron neutrinos and anti-neutrinos. INFORMATION ON THE MASS HIERARCHY AND THE VALUE OF THE THIRD MIXING ANGLE. MEMPHYS EVENTS 19.3 - 27 MeV 142 – 248 e 12 - 50 MeV 12 - 19 e

12 Beta-beams boost 6 He C. Volpe, J Phys G 30 (2004). A new facility to produce pure and intense low energy neutrino beams (10-100 MeV, i.e.  = 5-14). Low energy 12 C 40 Ar 16 O Supernova e detection exploits neutrino scattering on nuclei: LENA (scintillator), GLACIER (liquid argon), MEMPHYS (water Cherenkov) A BETTER KNOWLEDGE OF NEUTRINO-NUCLEUS REQUIRED. New development for the EURISOL project, included in the FP6 Design Study (2005-2009) A remark

13 Conclusions et Perspectives L’astronomie neutrino apporte des informations cruciales dans l’étude des particules et des interactions fondamentales. Les neutrinos provenant d’une explosion future ou reliques pourraient etre observés dans les observatoires de prochaine génération (étude de faisabilité dans FP7).

14 CP VIOLATION (Thèse de Jérome Gava) Un premier travail a montré des effets importants. Diverses études sont à réaliser: - effets dans un observatoire - inclusion de l’interaction neutrino-neutrino. Conclusions et Perspectives Des études récentes ont montré que cette interaction modifie de façon profonde la propagation des neutrinos dans les supernovae (effet Mikheyev- Smirnov-Wolfenstein ou MSW étudié depuis les années 80).

15 Neutrinos reliques de supernovae On a étudié les potentialités quant à l’observation des neutrinos et des anti-neutrinos reliques dans les observatoires futurs. Des études théoriques poussées nécessaires pour affirmer les potentialités de découverte. Conclusions et Perspectives

16 Merci!

17 Earth detection m2m2 vacuum high   1 coeur core  1 fluxes at emission  e   10 V (  ) G F  e. e e e e W A = -  m 2 /4E cos 2  B = -  m 2 /4E sin 2  A potential is introduced due to the coupling with matter. Effet Mikheyev-Smirnov-Wolfenstein (MSW)