GLACIER: PhysicsProspects With A100 kton LiquidArgon Detector

Antonio BuenoUNIVERSIDAD DE GRANADA

A. Bueno U. de Granada

Institutions

Relevant references

ETHZ (CH) A. Badertscher, L. Knecht, M. Laffranchi, A. Meregaglia, M. Messina, P. Otiougova, A. Rubbia, J. Ulbricht

Granada University (Spain) A. Bueno, J. Lozano, S. Navas INP Krakow (Poland) A. Zalewska INR Moscow (Russia) S. Gninenko IPN Lyon (France) D. Autiero, Y. Déclais, J. Marteau Sheffield University (UK) N. Spooner Southampton University (UK) C. Beduz, Y. Yang University of Bern (CH) A. Ereditato US Katowice (Poland) J. Kisiel UPS Warszawa (Poland) E. Rondio UW Warszawa (Poland) D. Kielczewska UW Wroclaw (Poland) J. Sobczyk

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GLACIER

Perlite insulation

d ≈ 70 m

h =20 m

Electronic crates

Single 100 kton “boiling” cryogenic tanker with Argon refrigeration

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Detector Layout(Bi-phase operation)

LArE-fie

ld

Chargereadoutplane

GAr

UV &visiblelightreadout +race track

E≈ 1 kV/cm

E ≈ 3 kV/cmElectronicracks

Cathode (–2MV)

Extractiongrid

1. Charge imaging + scintillation + Cerenkov light readout2. Charge amplification to allow for extremely long drifts

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Argon production and filling

≈30 MWEstimated total plant power

817kW (assuming for Argon 478 kJ/kg)Ideal Argon liquefaction power

5%Assumed efficiency

16 MWEstimated Argon Liquefactionpower

2 years (assumed)Liquid Argon 1st filling time

12 MWEstimated power for Argonseparation

5%Assumed efficiency

8’500’000 m3/day ≈ (205 m)3 /dayAir volume equivalent (Ar 1%)

600kW (assuming for Argon 354 kJ/kg)Ideal power of separation ofArgon mixture

1,2 liters/second or 150 tons/dayLiquid Argon 1st filling rate85000 m3/dayArgon gas equivalent

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GLACIER Physics Potential Non-accelerator Physics

Neutrino Physics at accelerators

Supernovaneutrinos

Solarneutrinos

Nucleonstability

p→e++π0

Atmosphericneutrinos

Dark MatterReactorNeutrinos

Beta Beams ν FactorySuper Beams

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Neutrinos from SupernovaeEight solar mass equivalent

Supernova at 10 Kpc

380 νe CC fromneutronization burst

Diffuse (Relic) Supernova Neutrinos

Signal Bckgnd

JCAP 0408:001, 2004JCAP 0310:009, 2003hep-ph/0307244

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Solar Neutrinoshep-ex/0103008

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Stability of Ordinary Matterhep-ex/0103008

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Expected backgrounds forproton decay

hep-ex/0103008

p → e+π0

p → K+ν

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Indirect Dark Matter Detection WIMPs accumulate in

the center of the Sun They annihilate

producing among othersvery energetic νe

Excellent capability todetect highenergy νepointing tothe Sun

JCAP 0501:001, 2005

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Non-accelerator Physics

SUMMARY

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Accelerator neutrinosEXPECTED RATES AT A NEUTRINO FACTORY

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Sensitivity on Θ13Nucl. Phys. B589 (2000) 577

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Sensitivity on CP violation inthe leptonic sector

Nucl. Phys. B631 (2002) 239

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Back-Up

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Parameters for a tentativelayout

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Cost Estimate

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