models of the earth: thermal evolution and geoneutrino studies
DESCRIPTION
Models of the Earth: thermal evolution and Geoneutrino studies. Bill McDonough , Yu Huang and Ondřej Šrámek Geology, U Maryland Steve Dye , Natural Science, Hawaii Pacific U and Physics, U Hawaii Shijie Zhong , Physics, U Colorado Fabio Mantovani , Physics, U Ferrara, Italy. - PowerPoint PPT PresentationTRANSCRIPT
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Models of the Earth:thermal evolution and Geoneutrino studies
Bill McDonough, Yu Huang and Ondřej ŠrámekGeology, U Maryland
Steve Dye, Natural Science,Hawaii Pacific U and Physics, U Hawaii
Shijie Zhong, Physics, U Colorado
Fabio Mantovani, Physics, U Ferrara, Italy
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Earth Models Update: …just the last 6 months!
Campbell and O’Neill (March - 2012, Nature): “Evidence against a chondritic Earth”
Murakami et al (May - 2012, Nature): “…the lower mantle is enriched in silicon … consistent with the [CI] chondritic Earth model.”
Warren (Nov - 2011, EPSL): “Among known chondrite groups, EH yields a relatively close fit to the stable-isotopic composition of Earth.”
Zhang et al (March - 2012, Nature Geoscience): The Ti isotopic composition of the Earth and Moon overlaps that of enstatite chondrites.
Fitoussi and Bourdon (March - 2012, Science): “Si isotopes support the conclusion that Earth was not built solely from enstatite chondrites.”
- Compositional models differ widely, implying a factor of two difference in the U & Th content of the Earth
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Nature & amount of Earth’s thermal power radiogenic heating vs secular cooling
- abundance of heat producing elements (K, Th, U) in the Earth
- clues to planet formation processes
- amount of radiogenic power to drive mantle convection & plate tectonics
- is the mantle compositionally layered or have large structures?
Geoneutrino studies
estimates of BSE from 9TW to 36TW
constrains chondritic Earth models
estimates of mantle 1TW to 28TW
layers, LLSVP, superplume piles
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U content of BSE models• Nucelosynthesis: U/Si and Th/Si production probability
• Solar photosphere: matches C1 carbonaceous chondrites
• Estimate from Chondrites: ~11ppb planet (16 ppb in BSE)
• Heat flow: secular cooling vs radiogenic contribution… ?
• Modeling composition: which chondrite should we use?
A brief (albeit biased) history of U estimates in BSE:•Urey (56) 16 ppb Turcotte & Schubert (82; 03) 31 ppb•Wasserburg et al (63) 33 ppb Hart & Zindler (86) 20.8 ppb•Ganapathy & Anders (74) 18 ppb McDonough & Sun (95) 20 ppb ± 20%•Ringwood (75) 20 ppb Allegre et al (95) 21 ppb•Jagoutz et al (79) 26 ppb Palme & O’Neill (03) 22 ppb ± 15%•Schubert et al (80) 31 ppb Lyubetskaya & Korenaga (05) 17 ppb ± 17%•Davies (80) 12-23 ppb O’Neill & Palme (08) 10 ppb •Wanke (81) 21 ppb Javoy et al (10) 12 ppb
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Heterogeneous mixtures of components with different formation temperatures and conditions
Planet: mix of metal, silicate, volatiles
What is the composition of the Earth? and where did this stuff come from?
MeteoriteNebula
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• Orbital and seismic (if available) constraints• Chondrites, primitive meteorites, are key• So too, the composition of the solar photosphere• Refractory elements (RE) in chondritic proportions• Absolute abundances of RE – model dependent• Mg, Fe, Si & O are non-refractory elements• Chemical gradient in solar system • Non-refractory elements: model dependent• U & Th are RE, whereas K is moderately volatile
“Standard” Planetary Model
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Iron meteorites
Stony Iron meteoritesAchondrites ~9%
Car-bonaceous Chondrites ~4%
Enstatite Chon-drites ~2%
Ordi-nary Chondrites 80%
Meteorite: Fall statistics(n=1101) (back to ~980 AD)
Most studied meteoritesfell to the Earth ≤0.5 Ma ago
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Mg/Si variation in the SSForsterite-high temperature-early crystallization-high Mg/Si-fewer volatile elements
Enstatite-lower temperature-later crystallization-low Mg/Si-more volatile elements
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Inner nebular regions of dust to be highly crystallized,
Outer region of one star has - equal amounts of pyroxene and olivine- while the inner regions are dominated by olivine.
Olivine-rich Ol & Pyx
Boekel et al (2004; Nature)
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EH
CI H
LL L
EL
Pyrolite-EARTH
CO
CM CV
Enstatite-EARTH
Olivine-rich
Pyroxene-rich
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EH
CI H
LL L
EL
EARTH
CO
CM CV
MARS
SS Grad
ients
-thermal-compositional-redox
Mars @ 2.5 AU Earth @ 1 AUOlivine-rich
Pyroxene-rich
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weight % elements
Fe
Si
Mg
Moles Fe + Si + Mg + O = ~93% Earth’s mass(with Ni, Al and Ca its >98%)
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CI and Si Normalized
Volatiles(alkali metals)
in Chondrites
Enstatite Chondrites-enriched in volatile elements-High 87Sr/86Sr [c.f. Earth]-40Ar enriched [c.f. Earth]
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What does this Nd data mean for the Earth?
• Solar S heterogeneous
• Chondrites are a guide
• Planets ≠ chondrites ?
Enstatitechondrites
Ordinarychondrites
Earth
CarbonaceouschondritesData from:
Gannoun et al (2011, PNAS)Carlson et al (Science, 2007)Andreasen & Sharma (Science, 2006)Boyet and Carlson (2005, Science)Jacobsen & Wasserburg (EPSL, 1984)
142mNd
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diagrams from Warren (2011, EPSL)
Enstatite chondritevs
Earth
Carbonaceouschondrites
Carbonaceouschondrites
Carbonaceouschondrites
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Earth is “like” an Enstatite Chondrite!
1) Mg/Si -- is very different
2) shared isotopic: O, Ti, Ni, Cr, Nd,.. 3) shared origins -- unlikely4) core composition -- no K, Th, U in core5) “Chondritic Earth” -- losing meaning…6) Javoy’s model – recommend modifications
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from McDonough & Sun, 1995
Th & UK
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U in the Earth: ~13 ng/g U in the Earth
Metallic sphere (core) <<<1 ng/g U
Silicate sphere 20* ng/g U
*Javoy et al (2010) predicts 12 ng/g*Turcotte & Schubert (2002) 31 ng/g
Continental Crust 1300 ng/g U
Mantle ~12 ng/g U
“Differentiation”
Chromatographic separationMantle melting & crust formation
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• Models with b ~ 0.3 --- Schubert et al ‘80; Davies ‘80; Turcotte et al ‘01• Models with b << 0.3 --- Jaupart et al ‘08; Korenaga ‘06; Grigne et al ‘05,’07
Thermal evolution of the mantle
Q Rab
Q: heat flux, Ra: Rayleigh number, b: an amplifer - balance between viscosity and heat dissipation
At what rate does the Earth dissipate its heat?
rogan (T1– T0)d3
h k
Ra =
h = viscosityr = densityg = accel. due gravitya = thermal exp. coeff.k = thermal diffusivityd = length scaleT = boundary layer ToRamantle > Racritical
mantle convects!
Parameterized Convection Models vigor of convection
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• Mantle convection models typically assume:mantle Urey ratio: ~0.7
• Geochemical models predict: mantle Urey ratio ~0.3
Convection Urey Ratio and Mantle Models
Urey ratio =radioactive heat production
heat loss
Factor of 2 discrepancy
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after Jaupart et al 2008 Treatise of Geophysics
Mantle cooling(18 TW)
Crust R*(8 ± 1 TW)
Mantle R*(12 ± 4 TW)
Core(~9 TW)
-
(4-15 TW)
Earth’s surface heat flow 46 ± 3 (47 ± 2)
(0.4 TW) Tidal dissipationChemical differentiation
*R radiogenic heat
total R*20 ± 4
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Plate Tectonics, Convection,Geodynamo
Radioactive decay driving the Earth’s engine!
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2005
2010
2011
DetectingGeoneutrinosfrom the Earth
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Terrestrial Antineutrinos
238U232Th40K
νe + p+ → n + e+
1.8 MeV Energy Threshold
212Bi
228Ac
232Th
1α, 1β
4α, 2β
208Pb
1α, 1β
νe
νe
2.3 MeV
2.1 MeV
238U
234Pa
214Bi
1α, 1β
5α, 2β
206Pb
2α, 3β
νe
νe2.3 MeV
3.3 MeV
40K 40Ca1β
Terrestrial antineutrinos from uranium and thorium are detectable
Efforts to detectK geonusunderway
31%
46% 20%
1%
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Reactor and Earth Signal
• KamLAND was designed to measure reactor antineutrinos.
• Reactor antineutrinos are the most significant contributor to the total signal.
KamLAND
Reactor Backgroundwith oscillation
Geoneutrinos
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Latest results
under construction
KamLAND
Borexino
106+29-28
from 2002 to Nov 2009
9.9 +4.1-3.4
from May ‘07 to Dec ‘09
Event rates
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Summary of geoneutrino results
MODELSCosmochemical: uses meteorites – Javoy et al (2010); Warren (2011)Geochemical: uses terrestrial rocks – McD & Sun, Palme & O’Neil, Allegre et alGeophysical: parameterized convection – Schubert et al; Davies; Turcotte et al; Anderson
Constrainting U & Th in the Earth
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Earth’s geoneutrino flux
X ( r 0) AX NX
2R
R
2dV aX ( r )r( r )
r r 02
X U or ThX(r0) Flux of anti-neutrinos from X at detector position r0
AX Frequency of radioactive decay of X per unit mass
NX Number of anti-neutrinos produced per decay of X
R Earth radius
aX(r) Concentration of X at position r
r(r) Density of earth at position r
Interrogating “thermo-mechanical pile” (super-plumes?) in the mantle …
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Present and future LS-detectors
SNO+, Canada (1kt) KamLAND, Japan (1kt)Borexino, Italy (0.6kt)
Hanohano, US ocean-based (10kt)
LENA,EU
(50kt)
Europe
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Constructing a 3-D reference model Earth
assigning chemical and physical states to Earth voxels
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Estimating the geoneutrino flux at SNO+
- Geology
- Geophysics
seismicx-section
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Global to Regional RRMSNO+SudburyCanada
using onlyglobal inputs
adding the regional geology
improving our flux models
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Structures in the mantle
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Testing Earth Models
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SUMMARY
Earth’s radiogenic (Th & U) power 20 ± 9 TW* (23 ± 10)
Prediction: models range from 11 to 28 TW
Future: -SNO+ online early 2013
…2020…?? - Hanohano - LENA
- Neutrino Tomography…