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LAGUNA. L arge A pparatus for G rand U nification and N eutrino A strophysics. Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM. Why ?. Neutrinos oscillations => New Particle Physics Main line besides future accelerator experiments

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Laguna

LAGUNA

Large Apparatus for Grand Unification and Neutrino Astrophysics

Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM


Laguna

Why ?

Neutrinos oscillations =>

New Particle Physics

  • Main line besides future accelerator experiments

  • Baryon number violation ? => Nucleon decay(Search for Proton Decay)

  • Baryon asymmetry  Leptogenesis ?

    Q13, CP violation in leptonic sector ?

    (Long Baseline Neutrino Experiments)


Astrophysics

Astrophysics

New Neutrino Observatories wanted Neutrinos as probes

  • Study of gravitational collapse(Supernova Neutrinos)

  • Study of star formation in the early universe (Diffuse Supernovae Neutrinos Background)

  • Precision study of thermonuclear fusion processes(Solar Neutrinos)

  • Test of geophysical models(Geoneutrinos)


Laguna

LENA

  • Low Energy Neutrino Astronomy

  • Diffuse Supernovae Neutrino Background

  • Supernova Neutrinos

  • Solar Neutrinos

  • Geoneutrinos

  • Proton Decay


Lena diffuse sn background

LENA: Diffuse SN Background

ne + p -> e+ + n

~25% of events are due to v’soriginating from SN @ z>1!

Rates depend on: supernova model, star formation rate, neutrino mass hierarchy

Range 20 to 220 / 10 years

“most probable” value ~ 100

Information on Supernova models & Star Formation rate (z~2)

M. Wurm et al., Phys. Rev D 75 (2007) 023007


Lena diffuse sn background1

LENA: Diffuse SN Background

  • optical measurements will determine the SNR with high accuracy

  • with this input, the spectral slope of the DSN can be used to distinguish between different SN explosion scenarios

comparison of count ratesin the energy bins10MeV < EB1 < 14MeV15MeV < EB2 < 25MeV


Lena supernova neutrinos

LENA: Supernova Neutrinos

Assumption: Supernova II with 8 solar masses at 10 kpc distance

ne flux and spectrum

ne flux and spectrum


Lena supernova neutrinos1

LENA: Supernova Neutrinos

Total neutrino flux

Total energy spectrum


Lena supernova neutrinos2

LENA: Supernova Neutrinos

Depending on threshold: p, nu - scattering dominated by

nmandnt

n + p -> n + p

Threshold ~ 50 pe

(photoelectrons)


Lena solar neutrinos

LENA: Solar Neutrinos

LENA Fiducial Volume for solar n: 18 x 103 m3

  • High statistic ( ~ 5.4 x 103 / day ) 7Be n + e ->n + e

  • test of small flux fluctuations in time

  • CNO and pep – neutrinos ( ~ 3 x 102 / day )

  • solar neutrino luminosity

  • contribution of CNO cycle to solar energy release

  • Charged current ne (13C,13N) e- reaction ( ~ 103 / year )

  • spectroscopy of 8B-n at energies below 5 MeV

  • (A. Ianni et al., hep-ph/0506171)


Lena solar neutrinos1

LENA: Solar Neutrinos

Non standard Interactions ?

(e.g. flavor changing neutral currents)

Standard MSW scenario

7Be pep CNO

8B

Friedland, Lunardini, Peña-Garay, hep-ph/0402266


Cno and the age of globular clusters

CNO and the age of Globular Clusters

  • 14N(p,g)15O new value? (new result from LUNA)

  • Prediction CNO-n altered by factor ~2

  • Age of Globular Clusters increased by factor 0.7 bis 1 Gy !

  • Measurement of CNO -n : determination of metallicity in the centre of the Sun


Lena solar neutrinos2

LENA: Solar Neutrinos

Electron recoil spectrum

Requirements:

low background levels in U, Th, 210Pb

at least ~4000 m.w.e. shielding


Lena geo neutrinos

LENA: Geo Neutrinos

  • Detection via inverse beta decay

  • measurement of radiogenic contribution to terrestrial heat (~ 40 TW)

  • test of the Bulk Silicate Earth model

  • test of unorthodox models of Earth‘s core (is there a breeder reactor ?)


Laguna

Rate of Geo-neutrinos in LENA

LENA @ Pyhäsalmi: ~ 1.5 x 103 events / year

Scaling KamLAND result to LENA:

between 3 x 102 and 3 x 103 events / year

Positron spectrum (arb. units)

Reactor BG

Uranium

Uranium + Thorium


Proton decay in supersymmetry su 5

Proton Decay in Supersymmetry SU(5)

  • GUT scale:

  • Preferred decay modes:

  • = (0.3 – 3) 1034y

    (S.Raby et al, 2002)

  • < 1035y

    (Babu, Pati, Wilzcek, 1998)


Proton decay non susy

Proton Decay(non SUSY)

(P. Nath 2006)

Limits from SuperKamiokande:


Lena proton decay

LENA: Proton Decay


Lena proton decay1

LENA: Proton Decay


Lena separartion e m like events

LENA: Separartion e- m-like events ?


Conclusions

Conclusions

  • LAGUNA – Design study for a large future European observatory (Water, Argon, Scintillator)

  • design study until ~ 2011

  • on APpec road map for Launch after design study completed

  • LENA – Physics Potential in Low Energy Neutrino Astronomy and Proton Decay

  • Proton Decay: T. Marrodan-Undagoitia et al., Phys. Rev. D 72 (2005) 075014

  • Geo-Nus: K.. Hochmuth et al., Astropart. Phys. 27 (2007) 21

  • DSNB: M. Wurm et al., Phys. Rev. D 75 (2007) 023007


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