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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

slide2
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)
slide10
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 ?)
slide21

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:

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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