hawaii , dec. 14-16, 2005 neutrino geophysics workshopjelena/post/hnsc/lindner... · 2005. 12....

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


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


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


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


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


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


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


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


• 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


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


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


Supernova Signal at SK

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

AccretionAccretionPhasePhase

KelvinKelvin--HelmholtzHelmholtzCooling PhaseCooling Phase


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


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


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


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


Reactor Neutrinos

identical detectors �� many errors cancel

E=4MeV �� 2km 4km 40km 80km

no degeneraciesno correlationsno matter effects

� KASKA� Braidwood� Angra, …

�Double Chooz


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


Sensitivity to sin22θθθθ13

Double Chooz

25 GW kt y


Improvement by Combining two Baselines

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


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


∆∆∆∆m2sol for L=40km


∆∆∆∆m2sol for L=70km


sin2(2θθθθ12) for L=40km


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


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

hawaii , dec. 14-16, 2005 neutrino geophysics workshopjelena/post/hnsc/lindner... · 2005. 12....

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