Outline

DUSEL Experiment Development and Coordination (DEDC)Internal Design Review

July 16-18, 2008Steve Elliott, Derek Elsworth, Daniela Leitner, Larry Murdoch, Tullis C. Onstott and Hank Sobel

Homestake DUSEL Initial Suite of ExperimentsDUSEL Experiment Development and Coordination

Outline

• Introduction - DEDC, who, what, why, when

• Physics Experiments

– Science Themes

– Superset of ISExperiments

• Biology-Geoscience-Engineering Experiments

– Science Themes


• PHYS-BGE Linking Themes

– Science Themes


• Summary

The Path Ahead – ISE Preparation Timetable

Anticipated October

Anticipated December

July 16 2008


Physics Experiments at DUSEL

• Long Baseline Neutrino Beam/Nucleon Decay• Dark Matter• Neutrino-less Double Beta Decay• Solar Neutrinos• Nuclear Astrophysics• Energetic particle effectsExploratory programs• Gravity Waves• 1- km Vertical Space


Three Neutrino Picture

3

2

1

τ3τ2τ1

μ3μ2μ1

e3e2e1

τ

μ

e

ν

ν

ν

UUU

UUU

UUU

ν

ν

ν

3 independent parameters+ 1 complex phase12, 23

FlavorStates

MNSMaki-Nakagawa-Sakata

mixing matrixMass

eigenstates

The physical neutrino eg. is a mixture of eigenstates such that:

= UUUetc.


Remaining Questions

• Mass hierarchy?

• How small is 13?

• CP Violation?

• Absolute mass scale?

• Dirac or Majorana?

Solar ~7.9x10-5ev2

Solar ~7.9x10-5ev2

Atmospheric~2.5x10-3eV2

Atmospheric~2.5x10-3eV2

Smalle allowed

m1

LB-L


Neutrino Beam From Fermilab(Strongly indorsed by P5)

NUMI/HOMESTAKE

NUMI/MINOS

New Target Hall,Shaft, and Service

Building

1300km

To DUSEL


Long Baseline Physics Program Why DUSEL?

Can probe remaining unknown neutrino parameters.

• Neutrino interactions in the Earth probe the hierarchy.Need long travel distance1300 km distance offers a significant improvement.

• CP violation may be observable with intense neutrino and anti-neutrino beams.– CP violation may explain matter/anti-matter asymmetry

of the UniverseRates are low, need very large detectors.

• Large detectors and great depth allows additional rich physics program.Nucleon decay, Relic supernovae detection, Solar neutrinos


Water Cherenkov/Liquid Argon

Super-Kamiokande 50,000 ton Water

Cherenkov Detector in Japan

Too small, too close (295 km)

LAANDD: modular cubic evacuated

•Scale existing water detector up to >100kt modules

•Initial Argon proposal is for 5kt

•Staged approach investigating development issues

•Triggering, purification, TPC design, vessel design, electronics, depth


Sensitivity

Hierarchy 13 CP Violation

Initial sensitivity of 100 kt water detectorThe DUSEL 100kt detector is almost an order of magnitude better than NOA for mass hierarchy determination for same running.

Additionally, High Precision (~1%) Measurement of Sin2223, m223 with

Muon CC Events


S-4 Issues / Facility Needs

• Most important is identifiable rock mass for excavation. This information drives the designs. Need coring & engineering.

• For LAr:– Risk analysis for underground siting.– Ventilation– Controlled release studies– Freeze-thaw mitigation– Egress plan– Vessel/cavern configuration

• For Water:– Shape and size optimization– Geo-textile design– PMT size/number optimization– PMT pressure testing– PMT mounting

• Top down power estimate for water detector- First module: 50,000 channels at 10 W/channel, plus 40% for HVAC and 20% other power, for total of 840kW.


The Direct Detection of Dark Matter


Breakthroughs in cosmology have transformed our understanding of the Universe.

•Spiral galaxies•rotation curves

•Clusters & Superclusters•Weak gravitational lensing•Strong gravitational lensing•Galaxy velocities•X rays

•Large scale structure•Structure formation

•CMB anisotropy: WMAPEvidence for Dark matter now overwhelming – amount becoming precisely known


Despite this progress, the identity of dark matter remains a mystery

• Constraints on dark matter properties the bulk of dark matter cannot be any of the known particles.– One of the strongest pieces of evidence that the

current theory of fundamental particles and forces, is incomplete.

• Because dark matter is the dominant form of matter in the Universe, an understanding of its properties is essential to attempts to determine how galaxies formed and how the Universe evolved.– Dark matter therefore plays a central role in both

particle physics and cosmology, and the discovery of the identity of dark matter is among the most important goals in basic science today.


Experimental Challenges

Overall expected rate is very small • Large low-threshold detector to

discriminate against various backgrounds.

– WIMPs and neutrons scatter off nuclei.

– Photons scatter off electrons.

• Minimize radioactive contamination.

• Minimize external incoming radiation.

– Deep underground location

The WIMP “signal” is a low energy (10-100 keV) nuclear recoil.

In many supersymmetric models, the lightest supersymmetric particle is, stable, neutral, weakly-interacting, mass ~ 100 GeV. All the right properties for WIMP dark matter!

Existing Limits

1 evt/10 kg/month

1 evt/1 ton/month

Xe or Ge rate(Ar ~1/5 rate/mass)

1 evt/10 ton/month

4850ft DUSEL Goal

Pre DUSEL Goal

7400ft DUSEL Goal

TheoreticalModels


Dark Matter Working Group (DMWG)Co-Chairs: Akerib, Gaitskell + Sadoulet

Candidate ExperimentsLUX/ZEPLIN 4850 20 tonne liquid Xe TPC

SuperXENON 4850 20 tonne liquid Xe TPC

CLEAN 4850 50 tonne liquid Ar or Ne

Depleted Argon TPC 4850 10 tonne Ar TPC

Low Temperature Ge 7400 1-2 tonne Ge

COUP 4850 Freon Bubble Chamber (Not S4, but may enter S5)

Gas - Hi Pressure & Low Pressure (Directional)

R&D 4850TPC 7400

Not ISE, but require R&D space underground

For list of groups associated with each experiment see presentations posted at http://dmtools.brown.edu/DMWiki/index.php/DMWG_DUSEL_Lead_Meeting_080424


Double Beta Decayrequires massive Majorana neutrinos

EXO 1-tonne Ge

• Two detectors proposed for DUSEL: EXO and GERDA/MAJORANA, which use isotopes of 136Xe and 76Ge with very different and complementary techniques. More than one experiment is required because:–backgrounds are different–possible gamma lines will not produce false detection in multiple isotopes–Nuclear matrix elements are different for different isotopes–The underlying physics of neutrinoless double beta decay can only be elucidated by studying more than one isotope

0 G0 M02m

2

At least one neutrino has a mass >50 meV. These experiments will have a sensitivity below 50 meV.


Solar Neutrinos

eBubble40-atm Ne gas

Low-E track readoutS4 proposal for prototype

20 tons for pp search

CLEANLiquid Ne

Scintillation readout10 tons for pp search

LENS125 t Liquid scint.

10 t InScintillation readout10 tons for CC study

Is 13 different from zero?Time dependencies in the Sun’s opacity or energy production?Is there a subdominant energy source in the sun?Is the MSW mechanism correct?Do nuclear reactions fully account for the Sun’s energy output today?


Accelerator Laboratory for Nuclear Astrophysics (ALNA)

CollaboratorsMatthaeus Leitner LBNLPaul Vetter LBNLPeggy McMahan LBNLDaniela Leitner LBNLDamon Todd LBNLAni Aprahamian Notre DamePhilippe Collon Notre DameManoel Couder Notre DameJoachim Goerres Notre DameFrancesco Raiola Notre DameDaniel Schuermann Notre DameEd Stech Notre DameMichael Wiescher Notre DameXiao-Dong Tang Notre DameJose Alonso Sanford LabArthur Champagne UNCClaudio Ugalde UNCMichael Famiano WMUPeter Parker Yale

International interestPietro Corvisiero INFN Genova, ITPaulo Prati INFN Genova, ITHeide Costantini INFN Genova, ITLucio Gialanella Naples, ITGianluca Imbriani Naples, ITChristina Bordenau HH-NIPNE, RO

Two accelerators

400 kV CLAIRE350 kV-3 MV (Dynamitron, other option being studied)

ECR ion source for extended energy range (1MeV/u)

Energy overlap allows to consistently measure cross section over a wide energy range and allow reliable extrapolations

Address a wide range of nucleosynthesis cross sections

Flexibility would make it a unique facility world wide

S-4 500k$/year for 3 years

ISE Project cost 20-30 M$


Science Stellar evolution, Origin of Elements, Stellar Neutrino Sources, Nucleosynthesis

log (c)

O-ignition

Ne-ignition

Si-ignition

log

(Tc)

H-ignition

He-ignition

C-ignition

7

8

10

9

0 42 8 104 6

Neutron sources Large uncertainty in s-process element production and subsequent nucleosynthesis

• Cannot be addressed in the LUNA facility

e.g. 22Ne(,n)25Mg, 25Mg(,n)28Si…

Proposed initial experiments

3He()7Be stringent benchmark of the facility•Constrain “invisible energy production”•Constrain solar metallicity and temperature Determines solar neutrino flux measured by current and proposed neutrino oscillation experiments

Challenge: Reaction rates at stellar energy are tiny, Extrapolation carry substantial uncertainties

Underground Shields cosmic ray backgroundsUnprecedented beam intensities will allow to push level of accuracy


Astrophysics facility requirements

•Facilities Underground (4850 ft level) Standard Experimental Cavity of 45x20x20m3, low background rock, external shielding

–2 Accelerators with energy overlap (50keV to 3MeV), auxiliary beams lines and power supplies–Experimental hall, control area, counting area–Target preparation and low background counting

•Utilities–Power estimate about 500 kW–SF6 storage, LCW Cooling water,

Cryogenic equipment/cryogenics –Climate control of the cave environment

(humidity)

•Above ground areas–Machine shop area –Above ground office space and counting areas–Laboratory space for general use (experiment

and target preparation, detector testing)


Science: Low Background Counting

Facility will need to be defined and supported by the various experiments

S-4 Process will further define the facility

A Dedicated Facility for the Assay, Control, and Production of Low Radioactivity Materials has been recognized as an essential shared task from the beginning of the DUSEL process.


Exploratory ISE proposals 1km Vertical Space

• Gravity Wave Exploring 1-Hz region (outside the LIGO frequency band) of gravitational waves (merger of white dwarfs and massive black hole)– Why Underground? Seismic noise and gravity gradient noise

are among the major obstacles for reaching 1-Hz scale.

Unique vertical Laboratory space• Evacuated tube required

– NNbar Collaboration – Gravity waves by Atomic Interferometry– Mirror Matter Transition Search– Study of Diurnal Earth rotation

• 1km Vertical Space (clean room and climate control required) – Facility for physics of Cloud Formation

Extensive feasibility studies are still to be done


Final Thoughts – The Physics program is very rich and requires a deep underground laboratory

• DUSEL is a vital component of a continuing neutrino program.– The distance from Fermilab and the depth make for a world-leading

program.• The mega-tonne scale detector will significantly advance the search for

nucleon decay and evidence for grand unification.• Dark Matter experiments are growing larger and more sensitive. DUSEL

depth, space and infrastructure are necessary components in this program.

• Double-beta decay experiments will be sensitive to the atmospheric neutrino mass scale.

• Solar neutrinos provide a unique window into the Sun.• A Nuclear astrophysics underground accelerator experiment will help us

to understand the origin of the elements.

ARMA-NSF-NeSS Workshop

• Resource Recovery• Petroleum and Natural Gas Recovery• In Situ Mining• HDR/EGS• Potable Water Supply• Mining Hydrology

• Waste Containment/Disposal• Deep Waste Injection• Nuclear Waste Disposal• CO2 Sequestration• Cryogenic Storage/Petroleum/Gas

• Site Restoration• Aquifer Remediation

• Underground Construction• Civil Infrastructure• Mining • Underground Space• Secure Structures

Biology-Geoscience-EngineeringScience Plan & Societal Imperatives

Mainly GeoMechanics

Mainly GeoHydrology

Both GeoHydrology and GeoMechanics

Spatial scale, x,y,z

Depth, z ->

• 4D - Experiments within a block of rock (~km-scale) at depth and at in situ temperature and stress.

• Access to fluids and gas with minimal contamination for molecular studies.

• Capabilities to characterize the rock block at multiple scales.

• Access to controlled energy sources.

• Proximal access to clean laboratory, fabrication facilities and unique technologies.

Why DUSEL for BGE?Why DUSEL for BGE?

Time, t

BGE – Science Questions

• Dark Life (Biology)– How deep does life go?– Do biology and geology interact to shape the world underground?– How does subsurface microbial life evolve in isolation?– Did life on earth originate beneath the surface?– Is there life on earth as we don’t know it?

• Restless Earth (Geosciences)– What are the interactions among subsurface processes?– Are underground resources of drinking water safe and secure?– Can we forewarn of earthquakes?– Can we view complex underground processes in action?

• Ground Truth (Geoengineering)– What lies between boreholes?– How can technology lead to a safer underground?– How do water and heat flow deep underground?


The Path Ahead - Initial Suite of Experiments, Bio-Geo-Eng

• Baseline characterization (NSF-SGER: no S-4)

Larry Stetler (SDSMT), Cynthia Anderson (BHSU)

• Ambient rock deformation processes/Ambient flow, transport, biodiversity and microbial and geochemical activity/Ultra-deep biological observatory

David Boutt (U Mass), Tom Kieft (NM Tech), Herb Wang (U Wisc)

• Induced flow, transport and activity/Induced rock deformation

Leonid Germanovich (Georgia Tech) and Eric Sonnenthal (LBNL)

• Underground construction and mining

Charles Fairhurst (UMN) and Joe Labuz (UMN)

• CO2 sequestration/Resource extraction

Joe Wang (LBNL) and Jean-Claude Roegiers (U Oklahoma)

• Subsurface imaging and sensing

Steven Glaser (UC Berkeley)


Facility Needs - Summary

RossRossYatesYates

4850L

7400L

8000L

300 L

3650L

~16000+

2000L

Active Processes LabsFracture and Transport Lab

Ambient TransportFiber Optic Strain Network

Ultra-deep Borehole

Summary of Facilities and Infrastructure

Exploration borehole

Relocatable sensing arrays

LB Caverns Level

Ambient Behavior and Ultra-Deep Biological Observatory – Scale Effects

Spatial Scale, m

10-10

10-14

10-18

10210110010-1 103

Lab scale Field scale

Regional scale

?

Perm

eabili

ty,

m2

[e.g. Dershowitz, 2004]


Compelling Research Questions Connecting Geomechanics, Geohydrology, and Geomicrobiology

• How do geomechanical, hydrologic, thermal and geologic conditions control the distribution of life in the deep subsurface?

• How do those factors control microbial diversity, microbial activity and nutrients?

• How do state variables (stress, strain, temperature, and pore pressure) and constitutive properties (permeability, porosity, modulus, etc.) vary with scale (space, depth, time) in crystalline rock?

What controls deep life?


Proposed Experiments

• Ultra-deep Drilling– What factors control the distribution of life as functions of depth, temperature,

and rock type?

– What are the patterns in microbial diversity, microbial activity and nutrients as a function of depth?

• Scale Effects Experiment (SEE) – How are stress state and strength related to geologic heterogeneity and

anisotropy, fracture geometry, the pressure and flow of fluids? – How do the fracture network, stress state, and constitutive properties of

crystalline rocks affect the stability of tunnels, shafts, wellbores, and large, room-sized excavations?

• Dark Flow – What controls porosity and permeability with depth in crystalline rock? – What are the characteristics of fracture networks that conduct water?– Do patterns of microbial diversity reflect connectivity of fractures (e.g. can

microorganisms be used as a new type of particulate tracer)? • 4-D Hydromechanical Simulator

– To synthesize observations for site selection of cavern construction, borehole locations, and bioaugmentation/biostimulation experiments.


An Overarching Hypothesis: Fluid flow in a rock mass can be predicted if both the stress field and the fracture network are characterized at a range of spatial scales.

• What is the stress state and are some fractures critically stressed?

• How is the transmissivity of fractures affected by stress state?

• How have mining excavations altered the stress field and hydrology?

• How does stress state affect stability of tunnels, shafts, wellbores, and large, room-sized excavations?

• How do the stress and flow environment affect microbial identity, activity, and diversity?


Induced Displacements Due to Dewatering K: 5E-10 m/s


Conceptual diagram of fiber-optic displacement sensor network

Distributed Strain and Temperature (DST) measurements can be made over kilometers of distance in the mine. However, development work must be done to establish clamping techniques to the rock mass and compared with fiber-optic displacement sensors, such as those shown in the figures.


Induced Flow, Transport and Activity/Induced Rock DeformationThe Active Processes Laboratory

• Objective - to evaluate how – Fractures propagate and deform during fluid flow and changes in stress in rock– Faults initiate, heal, seal, and reactivate– Fractures interact to create networks – Scaling laws can apply to rock fracture processes – Heat, mass, and microbes are transported through fractures and the adjacent rock matrix– Chemical and microbially-mediated reactions are controlled by heat and mass transport– New technologies can improve the imaging of fractures and faults

• Why is DUSEL the best or only place this experiment can be done?Objectives can only be achieved by manipulating in situ conditions at large scales and depths, and then

directly observing results. Such experiments require– Substantial and specialized sub-surface infrastructure over many years– Excavating host rock in the vicinity of created faults and fractures

• Expected results and their significance– Improved understanding of seismicity– Advanced understanding of fractures and fracture networks

• Why is it important to do these experiments in the near future?– public safety – water supply– hydrocarbon production and geothermal energy recovery– waste remediation and disposal– CO2

sequestration and climate change


FRACTURE PROCESSES LAB

Create fractures in highly instrumented setting to characterize deformation processes, then use for transport experiments


Example: FAULT EXPERIMENT

Approach

Utilize large, natural in-situ stresses – currently, the only option

Create failure by reducing existing load


Concept

1. Create a pair of parallel lines of boreholes or slots normal to 3

2. Cooling by T reduces 3 and allows controlled modification of stress state between lines

3. Reduce 3 between boreholes until failure occurs


Fault experiments at 300 ft level

Cooling


Fracture surface

Heating

Fault experiments at 300 ft level

Homestake DUSEL Initial Suite of ExperimentsDUSEL Experiment Development and Coordination42

SUITE OF EXPERIMENT – RUPTURE & TRANSPORT

• Fracture propagation • Fluid flow in networks• Deformation of fractures• Faulting• Scaling of fracture energy• Transport and geochemical reactions in fractures• Pressure solution at fracture asperities• Hydrothermal convection - permeability changes

from mechanical and chemical processes• Microbiological processes during fracturing

Relation to Some DOE Grand ChallengesFocus Areas

• Multiphase fluid transport in geologic media

• Chemical migration processes

• Subsurface characterization

• Modeling and simulation of geologic processes

Grand Challenges

• Computational Thermodynamics of Complex Fluids and Solids

• Integrated characterization, modeling and monitoring of geologic systems

• Simulation of multi-scale systems for ultra long times

Priority Research Directions

• Mineral-water interface complexity and dynamics

• Nanoparticle and colloid physics and chemistry

• Dynamic imaging of flow and transport

• Transport properties and in situ characterization of fluid trapping, isolation and immobilization

• Fluid-induced rock deformation

• Biogeochemistry in extreme subsurface environments

[DOE, BES, 2007]

Underground Construction & MiningScale Effects in Geomechanics – Space and Time

Deformation

Time [10 ~ 10 years]

2

6

Forc

e

Forc

e Decreasingdeformationrat e

Deformation

1 2 3

4

5

Elasticity

Plasticity

Continuummechanics

Damagemecha-nics

Localization and disintegration

Elastic unloading

Energy excess(Seismic deformation)

Energy deficit(Aseismicdeformation)

Maximumdesign force

TIME

SIZE

Intact block

Single joint

Rock mass

“We don’t know the rock mass strength. That is why we need an International Society” Muller, 24 May 1962

Complete Load-Deformation Behavior

[Courtesy: C. Fairhurst]

[Elsworth and Fairhurst, NSF-S1, 2007]

[Fairhurst, 2004]


Science

Objectives:1. Fully integrate knowledge into the design and construction of a cavern

2. Develop methods of ground control to accommodate the large cavity design – e.g. control fracture of rock through preconditioning and blasting studies

Why DUSEL?Large in-situ stress, fractured rock mass, and large scale excavation


Proposed Experiments (Describe A+ Experiments in multiple slides: maybe 1 to 5 slides)

Cavern Design• Predesign• Construction including

mitigation for stresses• Long-term performance

Subsurface Imaging and SensingSteven D. Glaser, working group herdsman

Towards the full Homestake Transparent Earth Observatory – installation and operation of a full complement of seismic, tilt, and EM instrument stations

Steven Glaser, UC Berkeley, Bill Roggenthen, SDSMT, Lane Johnson, LBNL

EM Passive Imaging as a Hazards Assessment Methodology

Dante Fratta – University of Wisconsin-Madison

Examining seismic sources from micro to macro through multi-sensor inversion

Steven Glaser, UC Berkeley, Lane Johnson, LBNL, Bill Roggenthen, SDSMT

Active source experiment to study anisotropy

Gary Pavlis, Indiana University

Installation of the Rapid City long-period station at the Homestake

Lind S. Gee, scientist-in-charge USGS Albuquerque

Stress Monitoring with high precision seismic travel time measurements

Fenglin Niu, Rice U; Paul Silver Carnegie Institute, Tom Daley, LBNL

Rock motion observation and mapping for the LIGO Experiment

Riccardo DeSalvo, CalTech; Vik Mandic, UMN

3D, Time-Lapse Seismic Tomography for Imaging Overburden Changes due to Dewatering

Erik Westman, Virginia Tech

Advanced Imaging of Gravity Variations and Rock Structures

Don Pool, USGS, Phoenix; Joe Wang, LBNL

Understanding the complexity of the crustal Earth system

Christian Klose, Columbia University

Prototype Broadband Array for DUSEL Gary Pavlis, Indiana University

3D resistivity & self-potential monitoring of the mine dewatering phase

Burke Minsley; US Geological Survey, Denver

Advanced Sensing to Track Trapped Persons and to Maintain Underground Communications

Tom Regan, Sanford Lab at Homestake; Steven D. Glaser, UCB; Joe Wang, LBNL

3-D passive electromagnetics for structural imaging, anisotropy, and methodological studies

Paul Bedrosian, US Geological Survey, Denver

1) Develop deep in-situ seismic observatory for rapid imaging of dynamical geo-processes at depth.

2) Provide rock mass dynamics and safety information to miners and tunnelers

3) Provide an infrastructure for all earth scientists

4) Improve ability to detect and characterize underground structures and activity

Towards a Transparent Earth

Install an acoustic “microscope” surrounding the Homestake workings – 1st NSF funded DUSEL research

S.D. Glaser, UC, BerkeleyW. Roggenthen, SDSMTL.R. Johnson, E.L. Majer,

LBNL

signal

noise

Deep is Quiet, and Quiet is Good

Seismic Imaging of Subsurface Stress

The time-varying stress field at depth is perhaps the most crucial parameter for understanding the earthquake triggering process.The Speed of Seismic Waves is a Measures of Stress in Rocks. This holds at seismogenic depth and can be used as a “stress meter”.

Fenglin Niu, Rice UniversityP. G. Silver, Carnegie Institution of WashingtonT. Daley, Lawrence Berkeley National Lab

Why at Homestake?Stress changes at seismogenic depth could be more difficult to observe with conventional surface instruments.Temperature variation at surface is a large noise source in the electronics.Deep observation could avoid surface environmental effects, such as precipitation.Need a deep natural experiment site that bridges laboratory study and large scale seismic experiment.


PHYS-BGE Linking Themes

• Geoneutrinos [GRAFG]

• Whole body counting [NORM]

• Cross-cutting Applications [CCA]

• Petrology, ore deposits and structure [PODS]


Geoneutrino Radiometric Analysis For Geosciences [GRAFG]

Working Group Members• Group Leader/ Heat Producing Elements: P. ILA & Point of Contact

Earth, Atmospheric & Planetary Sciences Dept., Massachusetts Institute of Technology

• Heat Flow/Geophysics: W. GosnoldGeology and Geological Engineering, University of North Dakota

• Cosmic-ray Physics: G. I. Lykken, Physics Dept. University of North Dakota

• Antineutrino Detector Instrumentation: P. JagamSNO Collaboration, University of Guelph; Norm Group Organization, Guelph, Canada

with 9 additional members


Q: Why study geoneutrinos?The Disparity of Global Heat Flow Estimates

from Geochemistry versus Geophysics

Bulk Silicate EarthBulk Silicate EarthGeochemical ModelGeochemical Model

Predicts global radiogenic Predicts global radiogenic heat production ~ 19 TWheat production ~ 19 TW

Terrestrial Heat Flow Terrestrial Heat Flow Geophysics EstimatesGeophysics Estimates

Estimated heat flow fromEstimated heat flow fromthe Earth is ( 30 - 44 )TW the Earth is ( 30 - 44 )TW


Geoneutrino Radiometric Analysis For Geosciences[GRAFG] Approach Concepts

• Cross-sectional schematic of the conical field of view dividing the interior regions of the Earth from the detection point of view.

• The cones C1, C2, C3, C4 completely enclose the inner core, outer core, lower mantle, upper mantle regions in the interior of the Earth.


Detection of Geoneutrinos

Geoneutrino detectionAntineutrino target is typically a scintillator, but could be a light emitting radiator also.

The radiation emitted by the interaction of the antineutrinos with the target, sensed by the light sensors, gets converted eventually to an analytical signal.

The energy of the incident antineutrino should be above the interaction threshold energy of the target medium, for the antineutrino to be detected.

Geoneutrino Detector

Basic Schematic


OBJECTIVES

Employing an existing mobile antineutrino detector. SONGS1 antineutrino detector is already developed for testing reactor antineutrinos for the purpose of test ban treaty monitoring. CHOOZ and MuNu experiments are also conducted successfully. The 1-ton detector designed and tested for Comprehensive Test Ban Treaty applications may be available in the next six months for further tests in the context of detecting geoneutrinos.

1. Develop a radiometric metric method using antineutrinos from the Earth for in-situ determination of K, U and Th to demonstrate proof-of-concept.

2. Interface with high pressure and temperature geochemistry knowledge base regarding fractionation of K, U and Th in Earth's interior.

3. Refine the Bulk Silicate Earth model.


Expected results and their significance

In comparison with large detector proposals for investigating the radioactivity in the deep interior of the earth, the significance of our proposal is that the results are achieved in a shorter time and at a less cost. The larger detectors can improve the precision investing 5 times the time required getting the results by us and at 10 times the cost.

Groups who worked or working with larger detectors are also recommending detectors with directional sensitivity.

Advantage of 1 ton detectors is their potential surface deployment for other geoneutrino experiments.


Cross-cutting Applications (CCA)

Robert McTaggart (SDSU) Program Manager

Betsy Sutherland (BNL) Radiation Biology

Bruce Bleakley (SDSU) Radiation Biology

Neil Reese (SDSU) Underground Agriculture

Thomas Schumacher (SDSU) Underground Agriculture

Gary Anderson (SDSU) Algal Biomass

Peggy McMahan (LBNL) Microelectronics

with 12 other investigators.


Cross-cutting Applications (CCA)

• Radiation Biology Objectives– Study the effects of “chronic” low dose exposures on human and

mammalian cells in low background laboratory.– Examine the effects of radiation on deep life at Homestake.

• Underground Agriculture Objectives– Develop a testing center for sustainable agriculture technologies needed

for NASA missions to the Moon and Mars.– Grow transgenic crops in isolated environments for use in

biopharmaceutical production, etc.– Assist in making DUSEL a “green” laboratory (remediation of grey water,

heavy minerals).– Develop organic LED lighting system to reduce power needs and heat.

• Algal Biomass Objectives– To develop a photobioreactor to grow algae for applications such as

biofuel production.• Microelectronics Objectives

– Develop a low background laboratory for long term system testing of, for example, microelectronics, photovoltaics and LEDs


Naturally occurring radioactive isotopes + low background Whole Body Counters

Glen Lykken (UND) lead and 9 other PI’s using low background facility


Petrology, Ore Deposits & Structure - PODS

• Interested principals and collaboratorsColin J. Paterson (SDSMT)Michael P. Terry (SDSMT)Brennan Jordan (USD)Kelli A. McCormick (SDGS)Nuri Uzunlar (SDSMT)Maribeth H. Price (SDSMT)Alvis L. Lisenbee (SDSMT)Derric L. Iles (SDGS)

and 25 other investigators


Petrology, Ore Deposits & Structure - Science

• Objective: Fundamental Question–What are the respective roles of deformation and dynamothermal

metamorphism in the production of fluids (magma and hydrothermal) and their flow-paths in orogenic systems?

• Synergistic activities– Baseline characterization: proposed research to characterize rock chemistry

and mineralogy, and map structural patterns and fabrics in the rocks will contribute to the baseline characterization dataset.

– Ambient flow & Ultra-deep biological observatory: geologic characteristics of the core that this group produces will contribute to evaluating the fundamental question posed in this proposal. In turn, PODS offers the expertise in geology and local geologic knowledge that will aid in consultation on and interpretation of rock units that may be intersected.

– Induced flow and transport: Our proposed experiments of element mobilization and precipitation mechanisms contribute to the heater experiment.

– Geoneutrinos & Low background counting facility: geochemical characterization of core in the planned laboratory construction areas will provide data on the abundance of U, Th, K and other elements necessary to model shielding requirements for facility.

The Path Ahead – ISE Preparation Timetable

Anticipated October

Anticipated December

July 16 2008

DUSEL AttributesDUSEL Attributes

• DUSEL will represent an important facility with unparalleled attributes:DUSEL will represent an important facility with unparalleled attributes:– Long-term uninterrupted access to site Long-term uninterrupted access to site

(long term response of structures and active processes)(long term response of structures and active processes)– Access to unusual depth for important initiatives in deep science Access to unusual depth for important initiatives in deep science

(physics and bioscience)(physics and bioscience)– Broad access to a large volume of rock Broad access to a large volume of rock

(scale effects and transparent Earth)(scale effects and transparent Earth)

• A facility for world-class science and engineering science in:A facility for world-class science and engineering science in:– Physics and AstrophysicsPhysics and Astrophysics– Sub-surface Science and EngineeringSub-surface Science and Engineering

• Important societal impacts:Important societal impacts:– ConstructionConstruction– Energy and sustainabilityEnergy and sustainability– Resource recovery and sustainabilityResource recovery and sustainability– Natural Hazards…..Natural Hazards…..

Outline

Documents

subsurface imaging

structural imaging

complement of seismic

large scale seismic

lbnlem passive imaging

imaging overburden changes

situ seismic observatory

homestake steven