JGL at Geonu 2013 1 John Learned Univ of Hawaii Future Large Liquid Scintillator Experiments For Geonu Studies and Much More Presentation at Neutrino Geosciences Takayama 23 March 2013 ID: 265823
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23 March 2013
JGL at Geonu 2013
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John LearnedUniv. of Hawaii
Future Large Liquid Scintillator ExperimentsFor Geonu Studies and Much More
Presentation at Neutrino Geosciences, Takayama, 23 March 2013Slide2
13 April 2009
John Learned at Cornell
2Where do Neutrinos come from?We can study most of these with a deep ocean instrument!
AstrophysicalAccelerators Soon ?
Nuclear Reactors
(power stations, ships)
Particle Accelerator
Earth’s Atmosphere
(Cosmic Rays)
Sun
Supernovae
(star collapse)
SN 1987A
Earth’s
Composition
(Natural
Radioactivity)
Big Bang
(here 330
/cm
3
)
Indirect Evidence
Slide3
Why this is a wide interest project
A large deep underwater detector can address
almost all of these neutrino sources! Many of them simultaneously. Low and high energy searches do not interfere. Nor do searches for rare phenomena such as supernovae and proton decay.Such an instrument is not just one experiment yielding one number, but will supply a huge variety of results (and PhDs) and can engage a large scientific community.This is true in geology as well as particle physics and astrophysics23 March 2013JGL at Geonu 20133Slide4
Geology Involvement
Studies to decide on locations for detector:
Ocean bottom cores, region studies Development of pile and other models Best possible regional calculationsStudies on spectra expected: Close examination of U/Th decay chains and beta decays Pressure effects?Improvement of earth models: Tuning various models with working groups Crucial temperature and seismic studies in less know regions? Sharpening community focus on earth heat issues Engaging the whole Geo Community in a project touching many specialitiesSeeking lateral variation and possible explanations, hidden reservoirsWe need a large multidisciplinary team to put this all together, not just physicists.23 March 2013JGL at Geonu 20134Slide5
The Road to Geonu
Science23 March 2013
JGL at Geonu 20135 Know we need great mass detectors > kiloton scale -> megaton scale Only (presently) viable technology is large tanks of liquid scintillatorDifficult to resolve mantle from crust at continental locationsBest to be far from nuclear reactors = mid-oceanNeed to be deep to avoid background (>3km)Ocean offers potential for relocation to multiple sitesWe can start with what we have now, all technology exists Challenges to do even better and go further than just “local” geonu rate: Better scintillator (output, water based, attenuation length) New optical detectors, better coverage and time resolution Directionality? K40 nus from the earth?Slide6
Large Electron Anti-Neutrino Experiments*
Continuing Experiments
KamLAND 1 kT LS 2 kmwe 1 MeV Borexino 0.4 kT LS 3 kmwe 1 MeVNear Term SNO+ 1kT LS+ 4 kmwe 1 MeV SK (w/Gd?) 22kT H2O+Gd 2 kmwe 4 MeVProposed HyperK 600kT H2O+? 1.5 kmwe(?) 6 MeV DayaBay2 20kT LS 1.5 kmwe 1 MeV RENO50 5kT LS ? kmwe 1 MeV LENA 50kT LS 3 kmwe 1 MeV LBNE Homestake 17kT Lar 0 or 4 kmwe 100 MeV? Watchman 1kT H2O+Gd 0.3 kmwe 4 MeV Hanohano 10kT LS 2-5 kmwe 1 MeV23 March 2013
JGL at Geonu 20136*Neglecting MINOS and NOVA, INO and MiniBOONE detectors, not relevant to this discussion on MeV electron anti-neutrinos.(And also to keep the list manageable… herein.)Slide7
Rough Physics Domains of Large Nuebar
Experiments
PhysicsKLBXSNO+SK w/HKDB2RN50LENAHstk LAr*WatchHanoReactor Mon
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☻☻☻Reactor Hierarchy
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Geonu
Det.
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Geonu
Mantle
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☻☻☻☻IndirectDM
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SNnus☻☻
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Relic SN
nus
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No Nu
ββ☻☻☻☻☻☻☻☻☻☻☻☻☻☻☻LBNE θ13☻?☻☻☻☻☻☻☻☻☻☻☻☻☻?LBNECPV☻☻☻☻☻☻☻☻☻☻☻☻☻?PDK☻☻☻☻☻☻☻☻☻☻☻☻☻☻☻☻☻☻
23 March 2013
JGL at Geonu 2013
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* Assuming 37 kT and deepSlide8
13 April 2009
John Learned at Cornell
8Locations for Present & Possible Geonu ExperimentsColor indicates U/Th neutrino flux, mostly from crustKamland
SuperKHyperKBaksan
Hanohano
EARTH ?
LENA
SNO+
Borexino
LBNE
LAr
DayaBay2Slide9
13 April 2009
John Learned at Cornell
9Simulated Geoneutrino Origination PointsKamLAND
50% within 500km25% from Mantle
Assumes homogeneous mantle &no core source
In Mid-Ocean 70% Mantle30% Other
Sanshiro
EnomotoSlide10
13 April 2009
John Learned at Cornell
10Why we need Geonu measuements in the deep ocean to measure the Mantle ContributionSteve Dye
mantleMantleModels16-18 typical
12-39 extremeCrust OnlySlide11
13 April 2009
John Learned at Cornell
11With a deep ocean detector we could resolve aSingle Reactor Source at CMB
resolution to few km10 sample simulated 1 yr runs
1 GW source observed by 100 kT detector
can be cleaned upSlide12
13 April 2009
John Learned at Cornell
12What Next for Geonus?Measure gross fluxes from crust and mantleDiscover or set limits on georeactors.Better earth modelsExplore lateral homogeneityUse directionality for earth neutrino tomographyFollow the science….Slide13
Applied Neutrinos!
Program to Study Long Range Reactor Monitoring and Detection
Working with colleagues at UH, NGA and IAI in US.Studies using all available neutrino tools: Hypothetical large detectors (100kT class)Assume availability of new photodetectors (LAPPDS of the like)Use oscillations fully in analysisCalculate full backgrounds including earth model and detector depthUse full Max Liklihood, with Bayesian statisticsTest importance of directional detection (obvious answer: very big boost)Conclusions:
Works better than we had guessed… big paper in press in Physics Reports. Will show some pictures here.23 March 2013JGL at Geonu 201313Slide14
23 March 2013
JGL at Geonu 2013
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mTC Idea
Do imaging with (100 ps) fast timing, not optics (time reversal imaging).Small portable 2.2 liter scintillating cube,
Boron doped plastic.4 x 6 MCP (x64 pixels each) fast pixel detectors on surrounding faces
Get neutrino directionality.Reject noise on the fly.
~10/day anti-neutrino interactions (inverse beta decay signature) from power reactor (San
Onofre
).
13 cm
2.2 liter
First, testing out new technology for precise antineutrino detection at UHSlide15
23 March 2013
JGL at Geonu 2013
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mTC Virtues Small size avoids positron annihilation gammas which
smear resolution (Xo ~42 cm).... gammas mostly escape, permitting precise positron creation point location.
Fast pixel timing (<100ps) and fast pipeline processing of waveforms rejects background in real time.
Having many pixels plus use of first-in light permits
mm
precision in vertex locations.
Neutrino directionality via precision positron production
and neutron absorption locations.
No need for shielding (unlike other
detectors,
except very close to reactor
Feasible even in high noise environment, near reactor
vessel, at surface (
eg
. in a truck)
.
Plan to take to reactor summer 2013Slide16
23 March 2013
JGL at Geonu 2013
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Snapshot of the Fermat Surface for a Single Muon-likeTrack
Track
Huygens
wavelets
Incoherent sum
coincident with
Cherenkov surface:
Not polarized!
J. Learned arXiv:0902.4009v1Slide17
Time Reversal Image Reconstruction
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JGL at Geonu 2013
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Figure by Mich SakaiSlide18
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JGL at Geonu 2013
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JGL at Geonu 2013
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JGL at Geonu 2013
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Fitting the
Positron StreakSlide21
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Reactor Rate versus Range
66
kT water based detector, no cuts.300 MWth Reactor23 March 2013JGL at Geonu 2013
22Slide23
Where the Reactors Live
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JGL at Geonu 201323Slide24
Table of Backgrounds & Rates
23 March 2013
JGL at Geonu 201324Lasserre and friendsSlide25
Smart integration of
geonus illustration
23 March 2013JGL at Geonu 201325Slide26
Crust and Mantle versus Range
23 March 2013
JGL at Geonu 201326Slide27
Where Comes the
Geonus
?23 March 2013JGL at Geonu 201327Account for oscillations and energy smearingOne lesson of the study: oscillations are very important tool.NUDAR Slide28
Geonu and Reactor Spectra
location off Spain ~300km to nearest reactor
23 March 2013JGL at Geonu 201328Geonus rule!Slide29
Seeking a Reactor:
Where Comes the Background?
23 March 2013JGL at Geonu 201329Sum of backgroundsSpectrum of backgroundsSlide30
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JGL at Geonu 2013
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Finding a Reactor and Power Output
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JGL at Geonu 201331Slide32
13 April 2009
John Learned at Cornell
32Future Geonu Dreams: Directional SensitivityDirectional information provides:・Rejection of backgrounds・
Separation of crust and mantle・Earth tomography by multiple detectorsGood News:
・Recoiled neutron remembers direction
Bad News:・Thermalization blurs the info・Gamma diffusion spoils the info・
Reconstruction resolution is too poor
Wish List:
・
large neutron capture cross-section
・
(heavy) charged particle emission &
・
good resolution detector (~1cm)Slide33
Increased angular resolution buys a lot
23 March 2013
JGL at Geonu 201333Slide34
13 April 2009
John Learned at Cornell
34Hanohanoa mobile deep ocean detector10 kiloton liquid scintillationUp to ~100
kt possibleDeploy and retrieve from bargeMeasure electron antinus for:Geophysics
Particle physics (hierarchy, mixing parameters)Remote reactor monitoring for anti-proliferation.And lots more science…Results from DARPA funded study, employingMakai Ocean Engineering for preliminary designand feasibility study. Slide35
13 April 2009
John Learned at Cornell
35Deployment SketchHanohano Engineering StudiesMakai Ocean EngineeringStudied vessel design up to 100 kilotons, based upon cost, stability, and construction ease.Construct in shipyardFill/test in portTow to site, can traverse Panama CanalDeploy ~4-5 km depthRecover, repair or relocate, and redeploy
Descent/ascent 39 min
Barge 112 m long x 23.3 wideSlide36
13 April 2009
John Learned at Cornell
36Addressing Technology IssuesScintillating oil studies in labP=450 atm, T=0°CTesting PC, PXE, LAB and dodecaneNo problems so far, LAB favorite… optimization neededImplosion studies Design with energy absorptionComputer modeling & at seaNo stoppersPower and comm, no problemsOptical detector, prototypes OKNeed second round design
20m x 35m
fiducial vol.
1 m oil
2m pure waterSlide37
13 April 2009
John Learned at Cornell
372 Candidate Off-shore Nuclear Power Reactor Sites for Physics
San Onofre, California- ~6 GWthMaanshan, Taiwan- ~5 GW
th
Can do unique studies of neutrino properties 50-60 km out from reactors.
Slide38
13 April 2009
John Learned at Cornell
38Summary of Expected ResultsHanohano- 10 kt-1 yr ExposureNeutrino Geophysics- near HawaiiMantle flux U geoneutrinos to ~10%Heat flux ~15%Measure Th/U ratio to ~20%Rule out geo-reactor if P>0.3 TWNeutrino Oscillation Physics- ~55 km from reactorMeasure sin2 (θ12) to few % w/ standard ½-cycleMeasure sin2(2θ13
) down to ~0.05 w/ multi-cycleΔm231 to less than 1% w/ multi-cycleMass hierarchy w/multi-cycle & no near detector; insensitive to background, systematic errors; complementary to Minos, NovaMuch other astrophysics and nucleon decay too….Slide39
13 April 2009
John Learned at Cornell
39Additional Physics/Astrophysics Hanohano will be biggest low energy neutrino detector (except for maybe LENA) Supernova Detection: special νe abilityRelic SN NeutrinosGRBs and other rare impulsive
sourcesExotic objects (monopoles, quark nuggets, etc.)Long list of ancillary, non-interfering science, with strong discovery potential
Broad gauge science and technology, a program not just a single experiment.Slide40
Other Applications for a large deep-water neutrino detector
Long Baseline with accelerators ~ 1
GeVHanohano with Tokai Beam (between Japan and Korea)?LENA with CERN beam??New LBNE Experiment with Fermilab Beam??Nucleon Decay (high free proton content)view details of decays such as Kaon modes Particle Astrophysics (low mass WIMPS,…)+ All the low energy physics (geonus, reactor studies, monitoring, solar neutrinos…..) unimpeded!23 March 2013JGL at Geonu 201340Slide41
What now?
We are ready to plan for a large deep ocean neutrino detector
To study geologyAnd much elseWe need a large interdisciplinary and multinational team to pull this offMany areas of expertise neededPlease consider how you can help
23 March 2013JGL at Geonu 201341