high mass indium detector for low energy solar neutrinos r. s. … · 2004. 2. 23. · eff% bs/in...

High Mass Indium Detector for Low Energy Solar Neutrinos

R. S. RaghavanBell Labs

NOON ’04, TokyoFeb 11, 2004

New U.S. Opportunities for Astroparticle Science & TechnologyAt Virginia Tech

Phase I: Virginia Tech Kimballton Lab for Underground Science & Engg

in the Kimballton Limestone Mine (1700 mwe)30 min from VT

Phase II: NUSEL @ Kimballton ?Engg. Studies initiated (VT Funded at $1.6 M )

Focus of Phase I

LENS (Low Energy Neutrino Science)Hi Mass Indium Detector of low energy νννν & νννν for Multidisciplinary Astroparticle Discovery

•Particle Physics, Astrophysics--Lo Energy Solar Nu

•High Red Shift Universe — Supernova Relic Nu

•Radiogenic Structure of the Earth — Geo-Nu

•White Paper: http://www.phys.vt.edu/~kimballton/

------MRI Proposal for LENS Supermodule Submitted to NSF

(BNL, INR Moscow, N. Carolina, Princeton, VT, other US…)

∆∆∆∆m2 = 7.1(0.4) eV2

tan2θθθθ12 12 12 12 =0.42(=0.42(=0.42(=0.42(5)Sin2θθθθ13 < 0.07 (3σσσσ)

•Solar Neutrinos Oscillate !

•Boron ????????????flux measured

•Neutrino parameters limited- LMA

Solar Neutrinos--What have we learnt so far?

•Solar Neutrinos Oscillate !

•Boron-8 solar νννν flux measured

•Neutrino parameters limited- LMABahcall & Penya-Garay ‘03

LMA basically from E( ν) ν) ν) ν) > 5 MeV---< 0.1% of total Flux

Parameter values from fit to

5 SN expts (νννν) + KamLand &

Chooz (νννν )

What Next ?•Low energy tests of high energy conclusions•Observe Main Energy Reaction of Sun--pp fusion

Need--Fully Resolved Lo Energy Solar ν ν ν ν spectrum

•Single Experiment•Single Solar Input—pp flux•Only NEUTRINO Data (No ν )ν )ν )ν )•PRECISION data--rates, Lo Nu fluxes•LoNu Discovery potential Goal Minimum loopholes, caveats

Definitive Neutrino, Sun

What‘s NewIn Exptlmethod ?

Bottom Line:

Finally : How does the Sun shine?–Direct Answer in School Books: Lo Nu Spectrum

LENS-Experimental Plan

LENS-SolLiquid scintillator basedCC Solar Nu Experiment at Kimballton (VA USA)(60ton In; 750 ton InLS; 3000 ton In-free LS)CC parameter Known only from (p,n) reactions.Direct measurement integral part of precision experiment.

LENS-Cal

Precision (<3%?) Calibration of In CC (GT) parameter

By MCi υ υ υ υ Source ( 37Ar ?) -- in BAKSAN, Russia

In metal foil/Plastic or LS Scint. Sandwich Detector

(5 ton In; 15 ton Scint)

Eve

nts

per

20

keV

E

ven

ts p

er 2

0 ke

V

Measured energy (MeV) Measured energyMeasured energy (MeV) Measured energy

pp Be

CNO pep

Nov 2003Nov 2003Nov 2003Nov 2003

0.5

Nov 2003Nov 2003Nov 2003Nov 2003

0.5

Be

CNO pep

Tagged electron Spectrum

pp

300 pe/MeV *

0 1.00 1.0

LENS-Sol-Goal

Solar Nu SpectrumAt <2 MeV to probe pp,pep, 7Be, CNO in Sun

ν spectrum e- spectrum

from

ν + Ι+ Ι+ Ι+ Ιn e- + 2 γγγγ +SnE(e-) = E(ν) ν) ν) ν) – 114 keV

e- tagged by isomeric 2 γ γ γ γ cascade decay ( τ ) τ ) τ ) τ )

•Update: Recent values •~ 440pe/MeV

ττττ e1 (prompt)

e/γγγγ2 2 2 2 (115)(115)(115)(115)

γγγγ3333(500)(500)(500)(500)In

Sn

νννν

pp 7Be pep CNO

SSM 29540 9200 480 2050

Practical =SSM x εεεε

7385ε ε ε ε =0.25

7360ε ε ε ε =0.8

380ε ε ε ε =0.8

1640ε ε ε ε =0.8

LMA =Prac x δδδδ

4800δδδδ=0.65

4300δδδδ=0.58

220δδδδ=0.58

930δδδδ=0.58

Design Event Rates for 60 ton Indium; 5y Livetime

Goals for Precision(including CC meas.):

pp: 3%: 7Be: 3%pep: 10% CNO ~6%

Specific expectations from Precision LoNu Results

•Proof of Physics of LMA -- νννν parameters ab initio

•Surprise Discovery? --Subdominant phenomena?

•SSM correct? -- (pp cycle--Be/pp ratio, CNO cycle)

•Nu- Luminosity vs. Photon Luminosity ---

Hidden energy sources in Sun?

Accessible only via Resolved Spectrum of

pp, Be, pep, CNO fluxes

LENS

LMA Favor Conversion

Main Feature :

Low energies: Vac

High energies: Matter

So far only hi energy Data

“ Smoking Gun” at:Low Energy

Schematic LMA ProfileBahcall & Pena-Garay (’03)

pp spectrum—0-420 keVpep line -- 1442 keV

PHYSICS of 2Nu-LMA with only low energy dataab initio measurement of sin22θθθθ & ∆∆∆∆m2

Approach: Measure flavor survival Pee of Individual Lo Nu features

Tools: Use ONLY Standard Candle fluxes: 1% prediction; Variable energy

7

0.75

0.8

0.85

0.9

0.95

1

4 6 8 10 12 14

K=

Pe

e/ [1

-0.5

sin

22

θθ θθ 12]

Sin2 2θθθθ12 =0.95

Sin2 2θθθθ12=0.7

Current LMA 95% c.l. area

7Be pep

pp

∆∆∆∆m2 (x105)eV2

Strategy for direct Measurement of Sin2θθθθ12 and ∆∆∆∆m2

At Low Energy:

pp directly givesSin2θθθθ12independent of ∆∆∆∆m2

Pep, Be lines at Higher energyReveal dependenceOn ∆∆∆∆m2

0.5

0.55

0.6

0.65

0.7

0.75

0.8

0.5 0.6 0.7 0.8 0.9 1

-

3%

Current limits from

7 experimentsLENS-Sol Only

0.5

0.55

0.6

0.65

0.7

0.75

0.8

0.5 0.6 0.7 0.8 0.9 1

-

3%

Current limits from7 expts

pp

flu

x in

LE

NS

-So

l /S

SM

Sin2 2θθθθ12

0.5

0.55

0.6

0.65

0.7

0.75

0.8

0.5 0.6 0.7 0.8 0.9 1

-

3%

Current limits from

7 experimentsLENS-Sol Only

0.5

0.55

0.6

0.65

0.7

0.75

0.8

0.5 0.6 0.7 0.8 0.9 1

-

±±±± 3%

Current limits 95%C.L.From 7 expts

pp

flu

x in

LE

NS

-So

l /S

SM

Sin212

Pee(pp:LMA)=0.985(1-0.5sin22θθθθ12)

Direct Measurement of Sin2θθθθ12 from pp data

0.5

0.55

0.6

0.65

0.7

0.75

4 6 10 12 148

sin22θθθθ =0.95

0.8

0.9

0.7

0.6

0.5

sin22θθθθ =0.95

0.8

0.9

0.7

0.6

0.5

∆∆∆∆m2 (x105)eV2

pep(

LEN

S-S

ol)/p

ep(S

SM

)

Current LMA limits 95% c.l. (7 expts)

Check of LMA with pep signal– Probe of Dm2

∆∆∆∆m2 (x105)eV2

0.4

0.45

0.5

0.55

0.6

0.65

0.7

0.75

4 6 8 10 12 14

sin22θθθθ =0.95

0.8

0.9

0.7

0.6

0.5

sin22θθθθ =0.95

0.8

0.9

0.7

0.6

0.5

Current LMA limits 95% c.l.(7 expts)

P ee(7 B

e)

Measurement of Model-Dependent Be flux using measured 7Be signal and 2νννν LMA determined from Pee of pp and pep stds

Std. Fluxes pp, pep –Assumed.Non-standard fluxes Be, pep, 8 B—derived

using Pee( 2νννν LMA) of pp and pep stds

Final Result: All original solar ν ν ν ν fluxes known.

Final tests of consistency of neutrino & solar physics: 3 neutrino mixing: θθθθ13 13 13 13 ????For solar Neutrinos: Pee (3nu) = Pee(2nu) cos4 θθθθ13

Derivation of SN fluxes from measured signals must use Pee(3νννν) rather than Pee(2νννν). If NOT,

all SN fluxes could be off by 10%since sin2θθθθ13 < 5% (3σσσσ) (Chooz).

To Explore Pee(3νννν):Use Measured Optical Luminosity L( γγγγ)& compare with Neutrino Luminosity L(νννν) derived from solar νννν Fluxes fromLENS-Sol using Pee(2νννν)

L(νννν) = L(γγγγ)[0.914φφφφp+ 0.07φφφφBe+ 0.014φφφφCNO] =cos4 θθθθ13 0.998L(γγγγ)ΦΦΦΦi from LENS (Pee(2νννν))δδδδ(φφφφpp) ~ ±±±± 3%;3%;3%;3%; δ(δ(δ(δ(L)<<1% δ(δ(δ(δ(φφφφΒεΒεΒεΒε) ∼) ∼) ∼) ∼±±±± 6%; 6%; 6%; 6%; δ(δ(δ(δ(φφφφCNO)∼)∼)∼)∼±±±± 10%10%10%10%

Equation anchored by L(γ γ γ γ ) to high precision. LHS precision determined basically by LENS δδδδ(φφφφpp) ±±±± 3%;3%;3%;3%; Inferences 1) Assume: L (ν)ν)ν)ν) ≡≡≡≡ L (γγγγ) → cos4 θθθθ13 < 0.03 → sin2 θθθθ13 < 0.015 (Particle phys)

2) Take sin2 θθθθ13 << 0.015 from future measurement → L(ν) = L(γ) tο ±±±± 3%;3%;3%;3%; (Solar Phys) Experimental Proof of solar energy = nuclear energy only ±±±±3%;

Final precision consistency of Neutrino and Solar Physics

Check other questions: Be/pp- ratio for Surprise Neutrino physics phenomenology?

Nunokowa: hep-ph/See also Smirnov ( )for low energy sterile conversion

Solar Astrophysics

Knowledge of Conversion Parameters implies Knowledge of solar Neutrino Fluxes correctedFor Conversion:All Fluxes known with high precision for the first timeCheck1) Solar Model Critically by individual predicted fluxes2) Check consistency of SSM using

Be/pp ratio = (3,3)/(3,4) He reaction ratio---backbone of SSM

3) Neutrino Luminosity Are there sources of Energy Of the sun BESIDES nuclear reactions?

115In ( 95.7%)ττττ = 6.4x1014 y

115Sn

B(GT) = 0.17; Qνννν=114

e1

(e/γγγγ)2 115.6 (e/γγγγ = 0.96)

γγγγ3 497.3

115 In(p,n)100.8 (e/γ =5.7)

ττττ = 4.76 µµµµs

ββββmax = 498.8

ττττ = 16 ps

τ = 231µs

9/2+

1/2+

3/2+

7/2+

11/2-

0

497.3

612.8

713.6

7/2+ 1857

B(GT) ~0.01; Qν =1362

e

115In ( 95.7%)ττττ = 6.4x1014 y

115Sn

B(GT) = 0.17; Qνννν=114

e1

(e/γγγγ)2 115.6 (e/γγγγ = 0.96)

γγγγ3 497.3

115 In(p,n)100.8 (e/γ =5.7)


ββββmax = 498.8

ττττ = 16 ps

τ = 231µs

9/2+

1/2+

3/2+

7/2+

11/2-

0

497.3

612.8

713.6

7/2+ 1857

B(GT) ~0.01; Qν =1362

e

The Indium Low Energy Neutrino Tag

115In ( 95.7%)ττττ = 6.4x1014 y

115Sn

B(GT) = 0.17; Qνννν=114

e1

(e/γγγγ)2 115.6 (e/γγγγ = 0.96)

γγγγ3 497.3

115 In(p,n)100.8 (e/γ =5.7)


ββββmax = 498.8

ττττ = 16 ps

τ = 231µs

9/2+

1/2+

3/2+

7/2+

11/2-

0

497.3

612.8

713.6

7/2+ 1857

B(GT) ~0.01; Qν =1362

e

115In ( 95.7%)ττττ = 6.4x1014 y

115Sn

B(GT) = 0.17; Qνννν=114

e1

(e/γγγγ)2 115.6 (e/γγγγ = 0.96)

γγγγ3 497.3

115 In(p,n)100.8 (e/γ =5.7)


ββββmax = 498.8

ττττ = 16 ps

τ = 231µs

9/2+

1/2+

3/2+

7/2+

11/2-

0

497.3

612.8

713.6

7/2+ 1857

B(GT) ~0.01; Qν =1362

e

The Indium Low Energy Neutrino Tag

random

νννν signal + Bgd at short delays

Bgd only at long delays (mostly 115In ββββ’s)

In

Hybrid In-Detector

Built-in live background measurement

BASIC METHODOLOGY

Foundations Laid by work of LENS R&D group 200-2003

In

In-free

Dcell

Dmin

Conceptual Hybrid Design to suppress In Bgd

Design parameters

• In =4t• Theor. Signal 1/d

• In betas >450 keV2.5x107

• pe/MeV=310

• DL (s) = 14 cm(@100 keV)

• Primary Cell???? 2s = 60 cm

• ????E (s) = 18 keV(@100 keV)

• Module Dim.10x10x300 (In)

Designparameters

In =4t•Theor. Signal 1/d

•In β β β β >450 keV: 2.5x1077

• pe/ /MeV =310∆∆∆∆L (σ)(σ)(σ)(σ)= 14 cm

@ 100 keV

• Primary Cell±2σ±2σ±2σ±2σ = 60 cm

• ∆∆∆∆E (σ)(σ)(σ)(σ)= 18 keV(@100 (keV)

•Module Dim.

10x10x300 (In)

Simulation

Sim. Results• hνννν = 6500/ MeV

Simulation of Spectroscopy in (old) Hybrid design

????????????(115 keV)γγγγ 3(500) γγγγ2 (115)

In

ττττ e1 (prompt)e/γγγγ2 2 2 2 (115)(115)(115)(115)

γγγγ 3333(500)(500)(500)(500)10x10x400 (with buffer)

Design parameters



• pe/MeV=310

• DL (s) = 14 cm(@100 keV)


• ????E (s) = 18 keV(@100 keV)


Designparameters


•In β β β β >450 keV: 2.5x1077

• pe/ /MeV =310∆∆∆∆L (σ)(σ)(σ)(σ)= 14 cm

@ 100 keV


• ∆∆∆∆E (σ)(σ)(σ)(σ)= 18 keV(@100 (keV)

•Module Dim.

10x10x300 (In)

Simulation


Design parameters



• pe/MeV=310

• DL (s) = 14 cm(@100 keV)


• ????E (s) = 18 keV(@100 keV)


Designparameters


•In β β β β >450 keV: 2.5x1077•In β β β β >450 keV: 2.5x1077

• pe/ /MeV =310∆∆∆∆L (σ)(σ)(σ)(σ)= 14 cm

@ 100 keV


• ∆∆∆∆E (σ)(σ)(σ)(σ)= 18 keV(@100 (keV)

•Module Dim.

10x10x300 (In)

Simulation



????????????(115 keV)γγγγ 3(500) γγγγ2 (115)

In


γγγγ 3333(500)(500)(500)(500)


????????????(115 keV)γγγγ 3(500) γγγγ2 (115)

In


γγγγ 3333(500)(500)(500)(500)


γγγγ 3333(500)(500)(500)(500)10x10x400 (with buffer)

J.P.Meyer (LENS Notes 2002-03

10x10x300 cm module; pp signal onlyEff% BS/In ββββ S N S/N

(10µµµµs)23 1.3x10-9 0.24 0.14 1.7

21 <0.7x10-9 0.22 <0> >3

Optimum Design Area

Eff. Be, CNO, pep signals

>80%; S/N >>1

Cell Size (cm)

εff.

4 6 8 10 12 14


(10µµµµs)23 1.3x10-9 0.24 0.14 1.7

21 <0.7x10-9 0.22 <0> >3

Optimum Design Area


>80%; S/N >>1


(10µµµµs)23 1.3x10-9 0.24 0.14 1.7

21 <0.7x10-9 0.22 <0> >3

Optimum Design Area


>80%; S/N >>1

Cell Size (cm)

εff.

4 6 8 10 12 14

J.P.Meyer, LENS Notes 2000-03

• · Hybrid strategy effective in solving the In -radioactivity background completely.

• · Granularity required of 60x10x10 cm vertex cell moderate and practical for high quality low energy nuclear spectroscopy

Conclusions of Analysis of Hybrid Design

• · Hybrid strategy effective in solving the In -radioactivity background completely.

• · Granularity required of 60x10x10 cm vertex cell moderate and practical for high quality low energy nuclear spectroscopy

Next Challenge: Design Hi-Mass Detector Next Challenge: Design Hi-Mass Detector

Conclusions of Analysis of Hybrid Design

• 1. High transparency InLS technology---optical length L(1/e) ~10m ---fewer InLS modules-- data channels—lower cost

• 2. Multi-layer reflecting foils ----New light pipe technology

- ----New design possibilities compatible to 1)

• 3. New hybrid design----Exploits 1) & 2)

Keystones to Hi-Mass In DetectorNew Developments 2003-04 (US-Russia)

0.01

0

0.004

0.008

0.012

0.016

0.02

0.024

0.028

370 400 430 460 490 520 550 580 610 640 670 700

Abso

rban

ce in

10

cm c

ell

Solvent PCInLS 7% In--No fluors

A(430) ~0.003→→→→L(1/e)(430) ~14m

Wavelength (nm)

0

0.004

0.008

0.012

0.016

0.02

0.024

0.028

370 400 430 460 490 520 550 580 610 640 670 700

Abso

rban

ce in

10

cm c

ell

Solvent PCInLS 7% In--No fluors

A(430) ~0.003→→→→L(1/e)(430) ~14m

Wavelength (nm)

In Liq. Scint.Solvent PCScint Yield 42% @7% wt InL(1/e)(430 nm)= 10 m

UpdateNew Safe Solvent:PhenylcyclohexaneF.P. 100CNon-toxicInLS/PCH Scint Yield 42% ofSolvent @ 7% InTransparency Same as PC

-0.005

0.005

0.015

0.025

0.035

470

Abs

orb

ance

in

10cm

cel

l

-0.005

0.005

0.015

0.025

0.035

370 420 520 570

Wavelength (nm)

InLS 7 wt % In/ PC solvent

No Fluors L(1/e) = 14 m

Fluors (pTP/MSB)L(1/e) (430) = 10 m

-0.005

0.005

0.015

0.025

0.035

470

Abs

orb

ance

in

10cm

cel

l

-0.005

0.005

0.015

0.025

0.035

370 420 520 570

Wavelength (nm)

InLS 7 wt % In/ PC solvent

No Fluors L(1/e) = 14 m

Fluors (pTP/MSB)L(1/e) (430) = 10 m

Data from BNL

Data from Bell Labs

Cage structure ofDouble sided 3M reflector foil 10x10cm Sq

Back reflector

Refl. foil light concentrator

End Buffer

20” PMT

3” PMT

InLS (8% In)400x10x10cm

InFree LS

Optical window

End Buffer50cm

z- Event coordinate fromTOF delay betweenfwd & bwd light

Back reflector

500 400

1010


Back reflector


End Buffer

20” PMT

3” PMT


InFree LS

Optical window

End Buffer50cm


Back reflector

500 400

1010


Back reflector


End Buffer

20” PMT

3” PMT


InFree LS

Optical window

End Buffer50cm


Back reflector


InFree LS

Optical window

End Buffer50cm


Back reflector

500 400

1010

2 ton Supermodule)LENS-Sol (Phase I-- )LENS-Sol (Phase I-- )

Hi Mass In Detector: In Mass 60 tonsIn LS (8% In) 750tonIn Free LS 3000 tonPMT:3” : 19000; 20” : 2100

50 100 150 200 250 300

Sig

ma

/ E (

keV

)

E,keV50 100 150 200 250 300

R=250 cm from PMT

E,keV

Performance Simulation of 1 –PMT Spectroscopy 500 cm

PMT Reflector

pe/MeV

50 100 150 200 250 300

E,keV50 100 150 200 250 300

00,000,020,040,060,080,100,120,140,160,180,200,22

00,000,020,040,060,080,100,120,140,160,180,200,22

0,000,020,040,060,080,100,120,140,160,180,200,22

00,000,020,040,060,080,100,120,140,160,180,200,22

0,000,020,040,060,080,100,120,140,160,180,200,22

00,000,020,040,060,080,100,120,140,160,180,200,22

0,000,020,040,060,080,100,120,140,160,180,200,22

R=250 cm from PMT

E,keV

Performance Simulation of 1 –PMT Spectroscopy 500 cm

PMT Reflector

σσσσ/ E =0.15

440 pe/MeV

LENS probe of other celestial bodies and phenomenaVia Antineutrino Spectroscopy via (ννννe bar,p)

LENS ideal device•Target Mass: 3750 tons•In content excellent n-detector (3000b)•Background suppressed because of short

time window for event search•Reactor background low (Preliminary estimate= ~300/3750 tons/y•Ideal combination of Hi Mass, Low bgd-----Likely the most powerful LOW ENERGYAntineutrino detector

Geo-Neutrinos:Global Measure ofU/Th in the Earth’s Crust:

Geo-Neutrinos:Global Measure ofU/Th in the

Detect Via antineutrinosEmitted in ββββ- decayOf U and Th

ννννe bar +p→→→→e+ +n

LENS-Sol 3.75kT(Lower ReactorBgd)

1kTLENS-Sol 3.75kT(Lower ReactorBgd)

1kTLENS-Sol 3.75kT(Lower ReactorBgd)

1kT

Super Nova Relic (Anti) Neutrino Sensitivity (Strigari et al)

VT Muon Telescope TentVT Muon Telescope Tent

Extra View Graphs

115In ( 95.7%)

115Sn

e1

115.6

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

νp

nττττ = 4.76= 4.76= 4.76= 4.76µµµµs

ττττ = 231 = 231 = 231 = 231 µµµµs

µµµµ100

11/2-

p

115In ( 95.7%)

115Sn

e1

115.6

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

115In ( 95.7%)

115Sn

e1

497.3

1/2+

3/2+

7/2+

0

497.3

612.8

νp

nττττ = 4.76= 4.76= 4.76= 4.76µµµµs

ττττ = 231 = 231 = 231 = 231 µµµµs

µµµµ100

11/2-

p

Cosmogenic production of In(p,n)Sn :

Rejectable via p recoil, n tagsRate @ 1600 mwe depth (Kimballton): I= 2x100/y/60t In;Tagged Background in solar runs = Iεεεε = ~50/y/60t

50-300

0

30

40

50

0.05 0.1 0.15 0.2 0.25 0.3

Energy, MeV

Sig

nal R

ate

20

10

LWO: ???? m 2 77x10 -12 eV2; sin22???? = 0.55

0

30

40

50

0.05 0.1 0.15 0.2 0.25 0.3

Energy, MeV

Sig

nal R

ate

20

10

LWO:

0

50

0.05 0.1 0.15 0.2 0.25 0.3

Energy, MeV

Sig

nal R

ate

0

50

0.05 0.1 0.15 0.2 0.25 0.3

Energy, MeV

Sig

nal R

ate

LWO:

400pe/ MeV

77x10 -12 eV2; sin22 = 0.55

30

40

20

10

30

40

20

10

∆∆∆∆m2 77x10 -12 eV2; sin22θ = 0.55400pe/ MeV

0

0.04

0.08

0.12

0 2 4 6 8 10 12 14Neutrino Energy (MeV)

Re

l. I

nte

ns

ity

SSM

LMA

LWO

LWO: Example ofSurpr ise scenar io.Energy spectrum and Pee>7 MeV identical to LMA

Revealed only byStrong oscillations ofpp spectrum

In-LS (5.5wt% In) PMTPMT

100 cm

5cm Source

241AmSum Coinc

57CoSum coinc

60 keV

26 keV

122 keV

Pb X-ray 136 keV

Borexino

Eurasian Crust

American Crust Pacific Crust

Atlantic Crust Kamland

Continental crust 35kmU 1.8ppm; Th 7.2ppm

Oceanic crust 6.5kmU 0.1ppm; Th 0.4 ppm

Total Heat 40TW(U+Th)Heat = 15TWNew: GeoReactor=3-10TW ?

Overall Geo Model: U,Th (Mantle) = U, Th (Crust);

HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE

MANTLEU 0.01ppmTh 0.04ppm

Total U: 8.2x1019 gTotal Th: 33x1019 g

Internal Energy Sources in the Ear th and their Distr ibution

Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



LENS @ Kimballton

Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



Internal Energy Sources in the Ear th and their Distr ibution

Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



Borexino

Eurasian Crust







HomestakeHawaii

2900 km

6400 km

South PoleGeomanda

R

CORE



LENS @ Kimballton

LENS-Sol (Phase I-- 20 ton In )

Supermodule

6300 InLS mod 10x10x4008% In

=20 ton In250 ton InLS

700 SuperMod

InFree LS = 60x60x500

-1440 kg LS=1000T LS

Total LS =1250 T

=

6300 3” PMT

700 20 “ PMT

Total=7000 Ch

.Double sided 3M Reflecting Foil Cage Structure

3” PMT for InLS Mod

20” PMT for In-Free LS Super Mod

10 10

60 cm

LENS-Sol (Phase I-- 20 ton In )

Supermodule

6300 InLS mod 10x10x4008% In

=20 ton In250 ton InLS

700 SuperMod

InFree LS = 60x60x500

-1440 kg LS=1000T LS

= 60x60x500-1440 kg LS=1000T LS

Total LS =1250 T

=

6300 3” PMT

700 20 “ PMT

Total=7000 Ch

6300 3” PMT

700 20 “ PMT

Total=7000 Ch

.Double sided 3M Reflecting Foil Cage Structure

3” PMT for InLS Mod

20” PMT for In-Free LS Super Mod

10 10

60 cm

high mass indium detector for low energy solar neutrinos r. s. … · 2004. 2. 23. · eff% bs/in...

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