GLACIER: Physics Prospects With A 100

kton Liquid Argon Detector

GLACIER: Physics Prospects With A 100

kton Liquid Argon Detector

Antonio BuenoUNIVERSIDAD DE GRANADA

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

A. Bueno U. de Granada

GLACIER

Perlite insulation

≈ 70 m

h =20 m

Electronic crates

Single 100 kton “boiling” cryogenic tanker with Argon refrigeration

A. Bueno U. de Granada

Detector Layout (Bi-phase operation)

LArE-f

ield

Charge readout plane

GAr

UV & visible light readout + race track

E≈ 1 kV/cm

E ≈ 3 kV/cm

Electronic racks

Cathode (–2MV)

Extraction grid

1. Charge imaging + scintillation + Cerenkov light readout

2. Charge amplification to allow for extremely long drifts

A. Bueno U. de Granada

Argon production and fillingLiquid Argon 1st filling time 2 years (assumed)

Liquid Argon 1st filling rate 1,2 liters/second or 150 tons/day

Argon gas equivalent 85000 m3/day

Air volume equivalent (Ar 1%)

8’500’000 m3/day ≈ (205 m)3 /day

Ideal power of separation of Argon mixture

600kW (assuming for Argon 354 kJ/kg)

Assumed efficiency 5%

Estimated power for Argon separation

12 MW

Ideal Argon liquefaction power

817kW (assuming for Argon 478 kJ/kg)

Assumed efficiency 5%

Estimated Argon Liquefaction power

16 MW

Estimated total plant power ≈30 MW

A. Bueno U. de Granada

GLACIER Physics Potential

Non-accelerator Physics

Neutrino Physics at accelerators

Supernova neutrinos

Solar neutrinos

Nucleon stability

pe++

Atmospheric

neutrinos Dark Matter

Reactor Neutrinos

Beta Beams

Factory

Super Beams

A. Bueno U. de Granada

Neutrinos from SupernovaeEight solar mass equivalent

Supernova at 10 Kpc

380 e CC from neutronization burst

Diffuse (Relic) Supernova Neutrinos

Signal Bckgnd

JCAP 0408:001, 2004

JCAP 0310:009, 2003

hep-ph/0307244

JCAP 0412:002, 2004

A. Bueno U. de Granada

Solar Neutrinoshep-ex/0103008

A. Bueno U. de Granada

Stability of Ordinary Matterhep-ex/0103008

A. Bueno U. de Granada

Expected backgrounds for proton decay

hep-ex/0103008

p e+0

p K+

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Indirect Dark Matter Detection WIMPs accumulate in

the center of the Sun They annihilate

producing among others very energetic e

Excellent capability to detect high energy e pointing to the Sun

JCAP 0501:001, 2005

A. Bueno U. de Granada

Non-accelerator Physics

SUMMARY

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Accelerator neutrinosEXPECTED RATES AT A NEUTRINO FACTORY

A. Bueno U. de Granada

Sensitivity on 13Nucl. Phys. B589 (2000) 577

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Sensitivity on CP violation in the leptonic sector

Nucl. Phys. B631 (2002) 239

A. Bueno U. de Granada

Back-Up

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Parameters for a tentative layout

A. Bueno U. de Granada

Cost Estimate

A. Bueno U. de Granada

A. Bueno U. de Granada