laguna
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/1.jpg)
LAGUNA
Large Apparatus for Grand Unification and Neutrino AstrophysicsLaunch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM
![Page 2: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/2.jpg)
Why ?Neutrinos oscillations =>
New Particle Physics Main line besides future accelerator
experiments Baryon number violation ? => Nucleon
decay (Search for Proton Decay) Baryon asymmetry Leptogenesis ?
CP violation in leptonic sector ?(Long Baseline Neutrino Experiments)
![Page 3: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/3.jpg)
AstrophysicsNew 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)
![Page 4: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/4.jpg)
![Page 5: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/5.jpg)
![Page 6: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/6.jpg)
![Page 7: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/7.jpg)
![Page 8: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/8.jpg)
![Page 9: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/9.jpg)
![Page 10: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/10.jpg)
LENA
Low Energy Neutrino Astronomy Diffuse Supernovae Neutrino Background Supernova Neutrinos Solar Neutrinos Geoneutrinos Proton Decay
![Page 11: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/11.jpg)
LENA: Diffuse SN Backgrounde + 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
M. Wurm et al., Phys. Rev D 75 (2007) 023007
Information on Supernova models & Star Formation rate (z~2)
![Page 12: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/12.jpg)
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
![Page 13: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/13.jpg)
LENA: Supernova NeutrinosAssumption: Supernova II with 8 solar masses at 10 kpc distance
e flux and spectrum
e flux and spectrum
![Page 14: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/14.jpg)
LENA: Supernova Neutrinos
Total neutrino flux
Total energy spectrum
![Page 15: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/15.jpg)
LENA: Supernova Neutrinos
Depending on threshold: p, nu - scattering dominated by
and
pp
Threshold ~ 50 pe
(photoelectrons)
![Page 16: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/16.jpg)
LENA: Solar Neutrinos
• High statistic ( ~ 5.4 x 103 / day ) 7Be + e + 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 e (13C,13N) e- reaction ( ~ 103 / year )
spectroscopy of 8B- at energies below 5 MeV
(A. Ianni et al., hep-ph/0506171)
LENA Fiducial Volume for solar : 18 x 103 m3
![Page 17: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/17.jpg)
LENA: Solar Neutrinos
7Be pep CNO
8B
Standard MSW scenarioNon standard Interactions ?
(e.g. flavor changing neutral currents)
Friedland, Lunardini, Peña-Garay, hep-ph/0402266
![Page 18: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/18.jpg)
CNO and the age of Globular Clusters
14N(p,)15O new value? (new result from LUNA)
Prediction CNO- altered by factor ~2
Age of Globular Clusters increased by factor 0.7 bis 1 Gy !
Measurement of CNO - : determination of metallicity in the centre of the Sun
![Page 19: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/19.jpg)
LENA: Solar Neutrinos
Electron recoil spectrum
Requirements:
low background levels in U, Th, 210Pb
at least ~4000 m.w.e. shielding
![Page 20: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/20.jpg)
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 ?)
![Page 21: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/21.jpg)
LENA @ Pyhäsalmi: ~ 1.5 x 103 events / year
Scaling KamLAND result to LENA:
between 3 x 102 and 3 x 103 events / year
Rate of Geo-neutrinos in LENA
Positron spectrum (arb. units)
Uranium
Uranium + Thorium
Reactor BG
![Page 22: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/22.jpg)
Proton Decay in Supersymmetry SU(5)
GUT scale:
Preferred decay modes:
–y (S.Raby et al, 2002) y (Babu, Pati, Wilzcek, 1998)
![Page 23: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/23.jpg)
Proton Decay(non SUSY)
(P. Nath 2006)
Limits from SuperKamiokande:
![Page 24: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/24.jpg)
LENA: Proton Decay
![Page 25: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/25.jpg)
LENA: Proton Decay
![Page 26: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/26.jpg)
LENA: Separartion e- -like events ?
![Page 27: LAGUNA](https://reader036.vdocument.in/reader036/viewer/2022062500/56815810550346895dc57d82/html5/thumbnails/27.jpg)
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