Other Physics with Geo-Neutrino Detectors

M. LindnerTechnical University Munich

Neutrino Geophysics WorkshopHawaii , Dec. 14-16, 2005

Manfred Lindner Neutrino Geophysics 2

Neutrinos & New Physics

+

neutrino properties & particle physics

neutrinos as probes

Manfred Lindner Neutrino Geophysics 3

Motivation: Physics Beyond the SM

gauge bosons

Higgs

quarksleptons

experimental facts:Dark Matter Dark Energyneutrino massesbaryon asymetry:mνννν> 0

gauge hierarchy problemδδδδmH

2 ~ ΛΛΛΛ2

SUSY ~TeV

3 generations, fermion rep.many parameters (mi ,mixings)unification into GUTs

mνννν=(mD)TMR-1mD

~ΛΛΛΛGUT+seesaw

astrophysics& cosmology

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Topics• Geo-neutrinos

���� large & expensive detectors ���� other motivations• Proton decay (baryon number violation)• Supernova neutrinos (GR collapse of old stars)• Supernova relic neutrinos (star formation @ early U)• Solar neutrinos (CNO, pep, 7Be ���� stellar evolution)• Nuclear monitoring• Neutrino oscillations (���� precision flavour physics)

- solar- atmospheric- reactor neutrinos- neutrino beams

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Large LENA–like Detektors based on LiSci

Muonveto

~12000 Pms (50cm)

100m

30m

A possible location:Pyhäsalmi mine, Finnland~ 1450 m depthlow radioactivityaccess via trucks

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Liquid Scintillator Technology

Modern scintillators: e.g. PXE, or PXE/mineral oil mixture- non hazardous, flashpoint 145° C���� easy handling: transport by railway, loading by pipeline���� moderate security problem

- density 0.99- high light yield ���� low energy events- low U,Th background level ���� see weak sources- experience with BOREXINO – CTF @ Gran Sasso���� 372 pe / MeV @ 20% coverage���� attenuation length ~ 4 m @ 430 nm���� after purification: ~ 12 m (R&D for LENS)���� ~ 120 pe/MeV in LENA���� low energy threshold (sub-MeV)���� good resolution in energy and position reconstruction

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Proton Decay and GUTs

• SUSY GUT scale:

• Preferred decay modes:

• ττττ = (0.3 – 3) 1034 y S. Raby et al, 2002

• ττττ < 1035 yBabu, Pati, Wilzcek, 1998

• ττττ ~ (MGUT)5

�������� LENA sensitivity

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Proton Decay @ LENA• favoured decay mode in some SUSY theories: pp�������� K K νννννννν• K is invisible in Water Cherenkov detectors• K and K-decay visible in LENA• Time information � high efficiency

����−−−−>µ>µ>µ>µ νννν

K

event structure:- 3-fold coincidence- energy spectrum���� strong bg. rejection

• T. MarrodanDiploma Thesis 2005

• T.M. et al. hep-ph/0511230

12.8ns µµµµ decay: ~2.2µµµµs

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Atmosphericneutrino event

ν + Ν −> Ν‘ + µ

Typical background:

no signal seen (90%cl) ���� ττττ > 4 x 1034 y

Super Kamiokande limit ττττ > 2.3 x 1033 y�������� 41 events in 10y @ LENA (0.5 bg evts.)

Potential of LENA for p����Kνννν

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• SN IIa: Collaps of a typical star ���� ~1057 νννν‘s• ~99% of the energy in νννν‘s• νννν‘s essential for explosion• 3d simulations do not explode

(so far... 2d����3d, ����convection? ... )

Supernova Neutrinos

MSW: SN & Earth

Very sensitive to - finite θθθθ13 - sgn(∆∆∆∆m2)

Dighe, Smirnov

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2 possibilities:

Supernova

neutron star or black hole

Keeps cooling... abrupt end of νννν−−−−emission

• impressive signal of a black hole inneutrino light

• neutrino masses �������� edge of νννν-signal

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Supernovae & Gravitational Waves

gravitational wave emission ��������

quadrupol moment of the explosion

� additional information about galactic SN � global fits: optical + neutrinos + gravitational waves� neutrino properties + SN explosion dynamics� SN1987A: strongest constraints on large extra dimensions

Dimmelmeier, Font, Müller

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Supernova Signal at SK

Simulation for Super-Kamiokande SN signal at 10 kpcTotani, Sato, Dalhed & Wilson

AccretionAccretionPhasePhase

KelvinKelvin--HelmholtzHelmholtzCooling PhaseCooling Phase

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Amanda/IceCube as a Supernova Detector

Each optical module (OM) picks up Cherenkov light from its neighborhood SN ���� correlated “noise” between OMs

SN @ 8.5 kpcSignal inAmanda

SN @ 8.5 kpcSignal inIceCube

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Galactic Supernovae with LENAEvent rates for a typical type IIa SN at GC (~10 kpc)

protons). off scattering (elastic (6)electrons) off scattering (elastic (5)

MeV) 15.1 E(Q CC with (4)

MeV) 17.3 (Q (3)MeV) 13.4(Q (2)

MeV) 1.8 (Q (1)

x

xx

12*12*1212x

1212e

1212

ppee

CCNeCBeC

nep

x

x

e

e

+→++→+

==+→+→+

=+→+=+→+

=+→+

−−

−

+

+

νννν

γννννν

γ

���� ννννe spectroscopy ~ 65

NC �������� sensitive to all flavours

~ 4000~ 4000 and ~ 2200~ 2200

~7800

~ 480

ννννe spectroscopy_

���� detect all flavour, neutrinos and anti-neutrinos

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SN and Earth Matter Effects

WaterCherenkov

Sighe, SmirnovDighe, Keil, Raffelt

SN model independent modulations in the spectrum due to Earth matter effects�������� θθθθ13, sign(∆∆∆∆m2)

ννννe

scintillator = good resolution

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atmospheric neutrinosSNR neutrinos

reactor background@ SK@LENA

8B solar ννννehep solar ννννe

���� no bg. @ LENA

Supernova Relic Neutrinos

SK limit close to expectations

LENA:~9MeV threshold���� SRN: ~6 events / y ���� 60 / 10 years

���� information aboutstar formation rate @ early universe

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Reactor Neutrinos

identical detectors ���� many errors cancel

E=4MeV ���� 2km 4km 40km 80km

no degeneraciesno correlationsno matter effects

� KASKA� Braidwood� Angra, …

�Double Chooz

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Neuclear Reactors @ Geo-neutrino Detectors

• reactors anti-neutrinos are an unwanted background• huge rate���� high statistics reactor experiments���� for some time during existence of the detector

• a rescaling exercise:Double Chooz: 10t x 5GW x 5y = 0.25 GW kt yLENA=50kt x 200MW x 2.5y = 25 GW kt y

• different possibilities:- movable detectors- location where a power reactor turns on/off- mobile reactors

���� J. Kopp, ML, A. Merle, M. Rolinec, to appear

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Manfred Lindner Neutrino Geophysics 21

Sensitivity to sin22θθθθ13

Double Chooz

25 GW kt y

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Improvement by Combining two Baselines

5GW kt y , nuclear power ship scenario ���� combine 0th + 1st osc. maximum (1+2 OK)

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Solar Oscillation Parameters & Reactors

Ideal baseline: 55 km (���� KamLAND) additionally 40 and 70 km

Events/year for 25 GW t y- main channel: 1741- reactor background���� nearest power reactors @ Pyhaesalmi: 1509

- Geo ννννs U: 923- Geo ννννs Th: 783- assume various geo-neutrino flux errors

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∆∆∆∆m2sol for L=40km

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∆∆∆∆m2sol for L=70km

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sin2(2θθθθ12) for L=40km

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sin2(2θθθθ12) for L=55km

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sin2(2θθθθ12) for L=70km

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combined

R2D2 - Reactor Experiments• Symmetric reactors,detectors:

– R1, R2, D1, D2 - may be different– L11=L22 and L12=L21

• Separate events from R1 and R2– R1 and R2 on/off times– Neutron displacement

• Simplest case: 1d line-upHigh statistics:���� precise statistical separation���� N11, N21, N12, N22 � self-calibration: N11/N21=N22/N12

� �� oscillation

� stable against size, backgrounds, ...� Improved sensitivity

Rr

NNNN

4

4

12*2122*11 =

1,5cm

6cm

R1

at detector D1:

R2

Huber, ML, Schwetz

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Conclusions

• Geo-neutrinos: - interesting by itself- large & expensive detectors

���� multiple purpose experiments• Large LiSci detectors like LENA, HSD, EARTH,

Super-Hanohano, …���� address a broad physics program

• Different technologies- mega-ton water Cherenkov- large LiAr detectors- large LiSci

���� physics / price: large LiSci very promising