Workshop in Matsuyama, Japan
November 4-7, 2015
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  

The	
  Earth’s	
  Mantle	  and	
  Core	  Structure,	  Composition,	
  Evolution	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  
	
  

	
  
	
  

IndexA Revised Chronology of the Inner Solar System
R. Brasser, S. Mojzsis, S. Werner .........................................................................................................1
Giant Impacts and Terrestrial Planet Formation
H. Genda ...................................................................................................................................................2
Stable Isotope Evidence for Planetary Differentiation
A. Shahar, S. Elardo, J. Labidi, W. Mao, R. Caracas, E. Schauble..................................................3
Crystallization of Magma Oceans and Implications for Mantle Convection
S. Labrosse, Ch.-Ed. Boukaré, M. Bouffard, A. Morison, Y. Ricard, P.J. Tackley, R. Deguen,
T. Alboussière ..........................................................................................................................................4
Early Evolution and Dynamics of Earth from a Molten Initial Stage
D.L. Lourenço, P.J. Tackley ..................................................................................................................5
Metal-Silicate Partitioning of Chlorine: Implications for the Origin of Terrestrial Missing
Chlorine
H. Kuwahara, H. Gotou, N. Ogawa, A. Yamaguchi, T. Yagi, S. Sugita .........................................6
Geochemical Evidence for the Temporal Evolution of the Mantle Redox State:
Implications for the Volatile Outgassing
V. Stagno, S. Aulbach ............................................................................................................................7
Conductivity and Correlations at High Pressures in Fe and FeO
R.E. Cohen, P. Zhang, K. Haule ...........................................................................................................8Core Neon
M.A. Bouhifd, A.P. Jephcoat, D. Porcelli, S.P. Kelley......................................................................9Transport and Storage of Volatiles in the Mantle and Core
E. Ohtani .................................................................................................................................................10
From Star to Stone: What Really Makes an Exoplanet "Earth-like?"
C.T. Unterborn, W.R. Panero ..............................................................................................................11
Linear Analysis on the Onset of Thermal Convection of Highly Compressible Fluids with
Variable Physical Properties: Implications for the Mantle Convection of Super-Earths
M. Kameyama........................................................................................................................................12
Melting of Sahara 97072 Meteorite (EH3 Chondrite) at 12 GPa and VariableTemperatures
W. Du, T. Irifune ...................................................................................................................................13
Effective Temperature Condition in the Separation Process of the Core and Mantle
H. Ichikawa, J. Hernlund, S. Labrosse, M. Kameyama ...................................................................14
Effect of a Stratified Basal Magma Ocean on the Geodynamo
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M. Laneuville, J. Hernlund, S. Labrosse, N. Guttenberg.................................................................15
142

Nd/144Nd Isotope Systematics in the Early Earth and High-pressure Melting
Experiments of Primitive Peridotite
N. Kondo, T. Yoshino, K.N. Matsukage, T. Kogiso ........................................................................16
Ab initio Electrical Resistivity of hcp Iron at Earth’s inner Core Conditions
H. Dekura ...............................................................................................................................................17
Hugoniot and Temperature Measurements of H2O up to 260 GPa Under Laser-driven
Shock Loading
T. Kimura, N. Ozaki, T. Sano, T. Okuchi, T. Sano, K. Shimizu, K. Miyanishi, T. Terai, T.
Kakeshita, Y. Sakawa, R. Kodama .....................................................................................................18
High-pressure in situ X-ray Laminography Using Diamond Anvil Cell
R. Nomura, K. Uesugi ..........................................................................................................................19
Phase Relations of FeH at Earth’s Core Pressure
C. Kato, K. Ohta, K. Hirose, Y. Ohishi..............................................................................................20
The Eutectic Liquid Composition in the Fe-Fe3S Binary System at the Core Pressure Range
Y. Mori, S. Tateno, K. Hirose, G. Morard, Y. Ohishi......................................................................21
Some Thermodynamic Properties of Larnite (β-Ca2SiO4) Constrained by High T/PExperiment and/or Theoretical Simulation
Z.H. Xiong, X. Liu, S.R. Shieh ...........................................................................................................22

The Lower Mantle: A Seismological Perspective
B.L.N. Kennett.......................................................................................................................................23
Persistence of Strong Silica-Enriched Domains in the Earth's Lower Mantle
J.W. Hernlund, C. Houser, M.D. Ballmer, R. Wentzcovitch, K. Hirose .......................................24
Discovery of New Iron Oxide Fe7O9 and Its Solid Solution, (Mg,Fe2+)3Fe3+4O9
R. Sinmyo, E. Bykova, S.V. Ovsyannikov, C. McCammon, I. Kupenko, L. Ismailova,
L. Dubrovinsky ......................................................................................................................................25
Helium Diffusion in Mantle Minerals from First Principles
J. Brodholt ..............................................................................................................................................26
Modes of Slab Behavior: from the Transition Zone to the Mid-Lower Mantle
C.R. Bina, H. Čížková ..........................................................................................................................27
Multiscale Seismic Tomography and Mantle Dynamics
D.P. Zhao ................................................................................................................................................28
Three-dimensional Analysis of Pore Effect on Composite Elasticity by Means of Finite
Element Method
A. Yoneda...............................................................................................................................................29
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Semi Analytical Model for the Effective Grain Size Profile in the Mantle of the Earth
A. Rozel, G. Golabek, M. Thielmann, P.J. Tackley .........................................................................30
The Relationship of Crystallographic Orientation between Perovskite and Post-Perovskite
During Phase Transformation
D. Yamazaki, M. Murakami, F. Xu, N. Hirao, Y. Seto ...................................................................31
Temperature of the Lower Mantle
C. Houser, J. Hernlund, R. Wentzcovitch, J. Valencia-Cardona ....................................................32
Waveform Inversion for 3D Structure in D"
K. Kawai .................................................................................................................................................33
Adjacent High- and Low-Velocity Regions around the Western Edge of the Pacific
Large-Low Shear Velocity Province
S. Tanaka ................................................................................................................................................34
Technical Developments on Acoustic Emissions Monitoring at High Pressures
T. Ohuchi, X. Lei, Y. Higo, Y. Tange, T. Irifune .............................................................................35
Creep Behavior of Fe-bearing Olivine under Hydrous Conditions
M. Tasaka, M.E. Zimmerman, D.L. Kohlstedt .................................................................................36
Stability Region of the (K, Na)AlSi3O8 Hollandite Solid Solution
Y. Zhou, T. Irifune, H. Ohfuji, T. Shinmei, W. Du ..........................................................................37
Direct Sound Velocity Measurements of Pyrolite Across the Mantle Transition Region
S. Gréaux, T. Irifune, M. Nishi, Y. Higo, T. Inoue, T. Arimoto, Z. Liu .......................................38
Effects of the Subducted Slab on Dynamics of the Lowermost Mantle
T. Kaneko, T. Nakakuki .......................................................................................................................39
Single Crystal Elasticity of the Lower Mantle Minerals using Inelastic X-ray Scattering
H. Fukui, A. Yoneda, A.Q.R. Baron ..................................................................................................40
Thermal Equation of State of MgSiO3 Post-perovskite
T. Sakai, H. Dekura, N. Hirao .............................................................................................................41
Experimental Identification of a New Pyrite-type Hydroxide at Multimegabar Pressures
M. Nishi, Y. Kuwayama, J. Tsuchiya.................................................................................................42
Technical Developments in High Temperature Generation with Sintered Diamond Anvils
T. Arimoto, T. Irifune, M. Nishi, Y. Tange, T. Kunimoto ..............................................................43
Over 3000°C Generation in Kawai-Cell Byboron-Doped Diamond Cylinder Heater
L.J. Xie, A. Yoneda, E. Ito...................................................................................................................44
Properties of Liquid Iron Alloys under Extreme Conditions
G. Morard, D. Andrault, D. Antonangeli, J. Siebert, F. Guyot, A.L. Auzende, O. Lord,
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J. Bouchet, M. Harmand, B. Cochain, G. Garbarino, I. Kantor, R.Torchio, E. Boulard,
M. Mezouar ............................................................................................................................................45
Liquid Iron Alloys with Hydrogen at Outer Core Conditions by First Principles
K. Umemoto, K. Hirose........................................................................................................................46
Core Liquids: Fact and Fiction
G. Helffrich ............................................................................................................................................47
Crystallization of SiO2 in Earth's Core after High-temperature Core Formation
K. Hirose, G. Morard, H. Ozawa, G. Helffrich, J. Hernlund ..........................................................48
Linking Seismic Observations of Earth's Inner Core Boundary to Deeper Structure
L. Waszek, A. Deuss, H. Godwin .......................................................................................................49
Freezing and Melting above the Inner Core Boundary
M. Lasbleis, J. Hernlund, S. Labrosse ................................................................................................50
Thermal Structure of the Inner Core Boundary in Numerical Dynamos
H. Matsui ................................................................................................................................................51
Lattice Preferred Orientation of Hcp-Iron Induced by Shear Deformation
Y. Nishihara, T. Ohuchi, T. Kawazoe, G. Maruyama, Y. Higo, K. Funakoshi, Y. Seto ............52
View and Perspectives on the Lower Mantle from Geo-neutrinos
S.T. Dye ..................................................................................................................................................53
Geo-neutrino Measurement with KamLAND and Future Prospects
H. Watanabe ...........................................................................................................................................54Core and Mantle Compositions: Neutrino Geophysics Insights
W.F. McDonough .................................................................................................................................55

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A Revised Chronology of the Inner Solar System
R. Brasser1, S. Mojzsis2, S. Werner3
1

ELSI, 2University of Colorado, Boulder, 3University of Oslo
Corresponding author’s email address: brasser@elsi.jp

Hadean (pre-3900 Ma) terrains are the oldest and most heavily cratered on the Moon,
Mercury and Mars [1], the latter two having crater densities comparable to the ancient highlandsof the Moon [1]. All three bodies were heavily bombarded during the first 600 million years of
the Solar System. Post-formation accretion has been suggested to follow a “Sawtooth” [2]intensity profile, but its precise timing remains elusive. From zircons and apetite crystals of lunar
samples, Martian and Vestan meteorites, NASA Curiosity isotope age measurements [3] and an
updated Martian crater chronology [4], the inner solar system likely experienced another intense
episode of bombardment long after the formation of the terrestrial planets [5]. The second ofthese has been dubbed the lunar cataclysm or Late Heavy Bombardment (LHB). Traditionallythe peak bombardment was thought to occur at 3.95 Ga, and recently the start has been pushed to
4.1 Ga[2], the supposed age of Nectaris basin. However, recent evidence shows Nectaris isolder[6], casting its timing into doubt. From the resetting and fracture ages of zircons on theMoon, Mars and Vesta, we determine the onset of the LHB to be near 4.3 Ga, after which thebombardment declined monotonically. We discuss the implications of this and construct a newtimeline for the evolution of the inner solar system.
References. [1] Werner, S. C. (2014): Earth and Planetary Science Letters, 400, 54; [2] Morbidelli, A., Marchi, S.,
Bottke, W.F., and Kring, D.A. (2012): Earth and Planetary Science Letters, 355, 144; [3] Farley, K. A. et al. (2014):
Science, 343, 1247; [4] Werner, S. C., Ody, A., and Poulet, F. (2014): Science, 343, 1343; [5] Bottke, W.F., et al.
(2012): Nature,485, 78; [6] Fischer-Godde, M., and Becker, H. (2011): Lunar and Planetary Science Conference, 42,
1414.

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Giant Impacts and Terrestrial Planet Formation
H. Genda
Earth-Life Science Institute, Tokyo Institute of Technology
Corresponding author’s email address: genda@elsi.jp
There are wide varieties of physical and chemical states among terrestrial planets in our solar
system, such as their sizes, orbits, spin states (also presence of moon), the amount andcomposition of atmosphere, the presence of ocean and life etc. How have these varieties been
built? Although the long-term evolutions on each planet are also important, here we focus on theformation stage of the terrestrial planets. This is because very energetic events occur during theplanet formation, such as the collisions among planetesimals [1, 2] and protoplanets [3, 4].
Especially, several tens of Mars-sized protoplanets collide with each other to form theterrestrial planets during the last stage of the terrestrial planet formation [5, 6, 7]. This stage iscalled the giant impact stage. Such energetic collisions should have a great influence on thevarious features of the terrestrial planets. For example, giant impacts are responsible for thecreation of the Moon [3,8] and the Martian satellites [9], and planets with extremely large coressuch as Mercury [10]. Giant impacts also affect volatile budget in terrestrial planets [11, 12], andleads to magma ocean [13]. Cooling of magmaocean and escape of water vapor results indifference in water content on Earth and Venus [14].
Even in extrasolar planetary systems, giant impact events are thought to be common.
Recently, thanks to infrared space telescopes such as Spitzer and AKARI, tens of warm debris
disks around solar-type (FGK) stars with ages of 107–108 yearshave been reported [15,16]. Thesewarm debris disks are estimated to be located roughly 1 AU to several AU from the central stars,
which corresponds to the terrestrial planet region in the solar system. Based on their stellar ages
and locations of the debris disks, the relation between these warm debris disks and giant impact
events has recently been discussed [17, 18, 19].
References. [1] Benz & Asphaug. (1999): Icarus, 142, 5–20; [2] Genda, H. et al. (2015): Icarus, 262, 58–66; [3]Canup. (2004): Annu. Rev. Astron. Astrophys, 42, 441–475; [4] Genda, Kokubo and Ida. (2012): Astrophys. J, 744,
137 (8pp); [5] Chambers. (2001): Icarus, 152, 205–224; [6] Kokubo and Genda. (2010): Astrophys. J. Lett, 714,
L21–L25; [7] Walsh, M. et al. (2011): Nature, 475, 206–209; [8] Genda and Abe. (2003): Earth Planets Space, 55,
53–57; [9] Citron, Genda and Ida. (2015): Icarus, 252, 334–338; [10] Benz. (2007): Space Sci. Rev, 132, 189–202.
[11] Genda and Abe. (2003): Icarus, 164, 149–162; [12] Genda and Abe.(2005): Nature, 433, 842–844; [13] Tonks
and Melosh. (1992): Icarus, 100, 326–346; [14] Hamano, Abe and Genda. (2013): Nature, 497, 607–610; [15]
Zuckerman, Rhee, Song and Bessell. (2011): Astrophys. J, 732, 61 (19pp); [16] Fujiwara, Ishihara, Onaka, et al.
(2013): Astron. Astrophy, 550, A45; [17] Jackson and Wyatt (2012): Mon. Not. R. Astron. Soc, 425, 657–679; [18]Melis, Zuckerman, Rhee, et al. (2012): Nature, 487, 74–76; [19] Genda, Kobayashi & Kokubo. (2015): Astrophys. J,
810, 136 (8pp).

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Stable Isotope Evidence for Planetary Differentiation
A. Shahar1, S. Elardo1, J. Labidi1, W. Mao2, R. Caracas3, E. Schauble4
1

Geophysical Laboratory, Carnegie Institution of Washington, 2Stanford University,
3
Ecole Normal Superieure de Lyon, 4University of California Los Angeles
Corresponding author’s email address: ashahar@ciw.edu

The differentiation of planetesimals occurred at high temperature, varying pressure, varying
oxygen fugacity and on bodies with varying compositions. As increasing knowledge points tothe Earth and other terrestrial bodies being formed by already differentiated planetesimals it isessential that we understand what these planetesimals looked like in order to fully understandhow the Earth and other terrestrial planets formed. In this study we focus on what we can learn
about the differentiation of planetesimals from stable isotope ratios.
During the differentiation process, the iron molten metal will alloy with other elements on its
route to the center of the planetary body. Which elements it bonds with will be a function of theconditions attending the core formation. For example, at high temperature under reducing
conditions Si is likely to alloy with iron, however, in more oxidizing conditions sulfur is likely toenter the metal. Determining which elements reside in planetary interiors requires indirect
methods such as high pressure and temperature experimental studies. The main candidates
considered are carbon, sulfur, oxygen, silicon and hydrogen.
We contend that by determining the equilibrium stable isotopic fractionation between metaland silicate we can provide an independent constraint on the composition of a planetary bodyand specifically address the likelihood of each light element in the core. The nature of the lightelement in an Fe-Ni core is directly related to the mode of formation, for example, whether
differentiation occurred at high pressure or low pressure, the redox conditions present, or thecomposition of the melt. Through high pressure and temperature experiments we cansystematically probe these variables and determine which are the most important in influencing
the stable isotope ratios found in natural samples today.

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Crystallization of Magma Oceans and Implications for Mantle Convection
S. Labrosse1, Ch.-Ed. Boukaré1, M. Bouffard1, A. Morison1, Y. Ricard1,
P.J. Tackley2, R. Deguen1, T. Alboussière1
1

ENS de Lyon, Univ. Lyon-1, France, 2ETH Zürich
Corresponding author’s email address: Stephane.labrosse@ens-lyon.fr
Classical models of magma ocean assumed that crystallization proceeded upwardly from thebottom because the pressure dependence of the liquidus is steeper than the liquid isentrope atmoderate pressure. Recent studies on high pressure melting of silicate show that this may nothave been the case and crystallization could have started from the mid-mantle [1, 2, 3]. The
dynamics and evolution following that initial crystal formation depends on the relative densities
of solids and liquids and of the density stratification in the solid resulting from crystallization. It
is likely that a significant upper part of the magma ocean fractionally crystallized from thebottom. Upon fractional crystallization, the liquid becomes enriched in FeO and so does the solidthat forms from it, leading to an unstably stratified solid mantle. If crystallization completes
before convection starts in the solid, its temperature at the end of crystallization follows thesolidus whose pressure and composition dependence make it super-isentropic. Therefore, bothcomposition and temperature stratifications in the mantle following a bottom-up crystallization
contribute in producing a Rayleigh-Taylor instability leading to an overturn of the solid mantle[4,5]. This overturn occurs very fast and leads to a stably stratified mantle with hot and FeO-poormaterial overlying cold and FeO-rich mantle. Thermal convection then resumes by cooling at thesurface of the solid mantle but has to overcome the initial stratification. Using a mantle
convection code (StagYY [6]) in which the initial conditions are those predicted for a bottom-up
magma ocean crystallization, we study the impact of various parameters (depth of initial
crystallization, partition coefficient of FeO, Rayleigh number) on the ability of mantle
convection to erase the initial stratification produced by magma ocean overturn.

References. [1] Fiquet, G. et al. (2010): Science, 329, 1516–1518; [2] Thomas, C.W. et al. (2012): J. Geophys. Res,
117, B10206; [3] Boukaré, C.-E., Ricard, Y., Fiquet, G. (2015): J. Geophys. Res, 120,6085–6101; [4] Hess, P.C. andParmentier, E.M. (1995): Earth Planet. Sci. Lett, 134, 501–504; [5] Elkins-Tanton, L.T., Parmentier, E.M. and Hess,
P.C. (2003): Meteoritics Planet. Sci, 38, 1753–1771; [6] Tackley, P.J. (2008): Phys. Earth Planet. Inter, 171, 7–18.

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Early Evolution and Dynamics of Earth from a Molten Initial Stage
D.L. Lourenço, P.J. Tackley
Institute of Geophysics, Department of Earth Sciences, ETH Zürich, Switzerland
Corresponding author’s email address: diogo.lourenco@erdw.ethz.ch
It is now well established that most of the terrestrial planets underwent a magma ocean stage
during their evolution. On Earth, it is probable that at the end of accretion, giant impacts like theMoon-forming impact, together with other sources of heat, melted a substantial part of the
mantle.
Considerable research has been done on magma oceans using simple 1-D models [e.g.: 1, 2,
3]. However, some aspects of the dynamics may not be adequately addressed in 1-D and require
the use of 2-D or 3-D models. Moreover, new developments in mineral physics that indicate thatmelt can be denser than solid at high pressures [e.g.: 4] can have very important impacts on theclassical views of the solidification of magma oceans [5].
The goal of our study is to understand and characterize the influence of melting on thelong-term thermo-chemical evolution of rocky planet interiors, starting from an initial molten
state (magma ocean). Our approach is to model viscous creep of the solid mantle, whileparameterizing processes that involve melt as previously done in 1-D models, including
melt-solid separation at all melt fractions, the use of an effective diffusivity to parameterizeturbulent mixing, coupling to a parameterized core heat balance and a radiative surface boundary
condition. These enhancements were made to the numerical code StagYY [6].
We will present results for the evolution of an Earth-like planet from a molten initial state topresent day, while testing the effect of uncertainties in parameters such as melt-solid density
differences, surface heat loss and efficiency of turbulent mixing. Our results show rapid coolingand crystallization until the rheological transition then much slower crystallization, large-scale
overturn well before full solidification, the formation and subduction of an early crust while apartially-molten upper mantle is still present, transitioning to mostly-solid-state long-term mantle
convection and plate tectonics or an episodic-lid regime.

References:[1] Abe, Y. (1997): PEPI, 100, 27-39; [2] Solomatov, V. S. (2007): Treat. Geophys, 9, 91-120; [3]Elkins-Tanton, L. T. (2008): EPSL, 271, 181-191; [4] de Koker, N., Karki, B. B., Stixrude, L. (2013): EPSL, 361,
58-63; [5] Labrosse, S, Hernlund, J. W, Coltice, N. (2007): Nature, 450, 866-869; [6] Tackley, P. J. (2008): PEPI,
171, 7-18.

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Metal-Silicate Partitioning of Chlorine: Implications for theOrigin of Terrestrial Missing Chlorine
H. Kuwahara1, H. Gotou2, N. Ogawa3, A. Yamaguchi3, T. Yagi4, and S. Sugita1,41Departmentof Complexity Science and Engineering, University of Tokyo
2
Institute for Solid State Physics, University of Tokyo
3
Atmosphere and Ocean Research Institute, University of Tokyo
4
Deptartment of Earth and Planetary Science, University of Tokyo
Corresponding author’s email address: kuwahara@astrobio.k.u-tokyo.ac.jp
The chlorine abundance of the bulk silicate Earth may be greatly depleted relative to theprediction based on various types of primitive materials, such as chondrites [1]. There are two
hypotheses for this depletion of terrestrial chlorine; Incorporation into the Earth’s core and acollisional erosion of primordial hydrosphere. Here we experimentally examine the possibility of
the former case. Specifically, the metal-silicate partitioning of chlorine in a magma ocean isinvestigated.
In this study, we experimentally determined the metal-silicate partition coefficient ofchlorine as functions of pressure and temperature. Starting materials were prepared from a
mixture of high-purity oxides (SiO2, Al2O3, CaO, MgO, FeO) and metal (Fe, FeS). The relative
abundances of each component in the silicate portion were assumed to be chondrites. Chlorine
was added to the mixture as FeCl2. The starting materials were enclosed in either a graphite
capsule or a single crystal MgO capsule. The experiments were performed at 4-23 GPa and1923-2673 K using the multi-anvil press. The chemical compositions of recovered samples wereanalyzed by wavelength-dispersive electron microprobe.
Our experimental results show that (1) chlorine is highly lithophile, (2) the metal-silicate
partition coefficient of chlorine increases with increasing temperature, and decreases withincreasing pressure. Based on the experimental results and thermodynamic consideration, we
estimated the metal-silicate partitioning of chlorine at the base of a magma ocean which becomesdeeper as accretion proceeds. The P-T conditions at the base of a magma ocean were assumed tobe the same as the peridotite melting curve. Calculation results show that the metal-silicate
partition coefficients of chlorine at the base of a magma ocean are much lower than the required
value proposed by Sharp & Draper [1]. Thus, Earth’s core is unlikely to be the origin of
terrestrial missing chlorine. Given that the fluid-melt	  partition coefficient of chlorine is ~10[e.g., 2], chlorine is likely to be partitioned into primordial hydrosphere. If this is the case,terrestrial missing chlorine may require an extensive loss of primordial atmospheres and oceans
during the main-accretion phase.

Reference. [1] Sharp, Z. D. and Draper, D. S. (2013): EarthPlanet. Sci. Lett, 369-370, 71-77; [2] Metrich, N. et al.
(2001): Journal of Petrology, 42, 1471-1490.

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Geochemical Evidence for the Temporal Evolution of the Mantle Redox State:
Implications for the Volatile Outgassing
V. Stagno1,2, S. Aulbach3
1

Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
2
Geodynamic Research Center, Ehime University, Matsuyama, Japan
3
Goethe Universität, Frankfurt, Germany

The oxidation state (fo2) of the interior of Earth has modulated the extraction of volatiles
from depth and their redistribution to the shallower portions of the planet and, eventually, to thehydrosphere and atmosphere through time. During core formation and crystallisation of theearly-Earth from a magma ocean, the reducing fO2 likely buffered by the equilibrium between theprimitive silicate melt and the percolating Fe metal promoting immobility of C-O-H gaseous
species; whereas presently fO2s between -1 and 0 log units (FMQ) as recorded by mid-ocean
ridges basalts (MORBs) can mobilize large amount of volatiles from depths of the lower/upper
mantle.
To date, several studies have interpreted similar oxidised conditions for mantle-derived
melts (komatiites, picrites, and basalts) from ~3800 Ma as evidence that the mantle fO2 has
attained its present value shortly after core formation and remained relatively constant over time.
Whether this increase was gradual or not, at least up to the Hadaean, remains debated andstrongly dependent on what mechanisms operated.
We use the V/Sc ratio of preserved Archean orogenic and mantle eclogites that have
low-pressure protoliths separated from a spinel peridotite source to unravel the redox history of
the convecting mantle. The mantle oxidation state in the Archaean convecting mantle andpossible implications for the speciation of volatiles is reviewed based on geochemical data
combined with thermodynamic predictions of the variation of fo2 as function of depth,
temperature and bulk composition.
This has several consequences such as, (1) the locus of a volatile-bearing peridotite solidus
and the composition of fluids/melts that formed along the mantle adiabat; (2) redox melting as aprecursor to continental rifting during which carbonatitic to carbonate-silicate melts might havebeen the first magmas to be erupted, and (3) the increase in atmospheric CO2 accompanied byfirst whiffs of oxygen.

Reference.[1] Li and Lee. (2004): EPSL, 228, 483-493; [2] Scaillet and Gaillard. (2011): Nature, 480, 48-49.

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Conductivity and Correlations at High Pressures in Fe and FeO
R.E. Cohen1,2, P. Zhang1,3, K. Haule4
1

Extreme Materials Initiative, Geophysical Laboratory, Carnegie Institution for Science,
Washington, D.C. USA
2
Department für Geo-und UmweltwissenschaftenLudwig-Maximilians-Universitaet,
Munich, Germany
3
Department of Physics, Xi'An Jiaotong University, Xi'an, Shaanxi, China
4
Deptartment of Physics, Rutgers University, USA
Corresponding author’s email address: rcohen@carnegiescience.edu

Under pressures in the Earth, iron in minerals behaves very differently from simple elements,
such as magnesium, even though Fe2+ and Mg2+ easily substitute for each other at low pressures.
I will discuss the behavior of FeO and Fe under high pressures and temperatures using modern
electronic structure methods. FeO is an insulator at ambient conditions, but at high pressures andtemperatures we found it becomes a metal [1]. We are investigating these properties using amethod beyond the standard model, density functional theory (DFT), for electronic structure. We
are using self-consistent DFT/Dynamical Mean Field Theory (DMFT)[2], which includes
quantum and thermal fluctuations, multiplets, and all-orders of local electronic correlations. We
find that electron correlations are important even in the generation of Earth’s magnetic field.
Earth's magnetic field was believed to arise from thermal convection of molten iron alloy in
Earth's outer core, but density functional theory (DFT) calculations suggested that the
conductivity of iron is too high to support thermal convection[3-6], so that new geodynamo
models were being developed[7, 8]. The DFT computations for resistivity were based on the
scattering of electrons off of atomic vibrations, or electron-phonon (e-p) scattering. We applied
self-consistent density functional theory plus dynamical mean-field theory (DFT+DMFT) [2] toiron and found that at high temperatures electron-electron (e-e) scattering is comparable to thee-p scattering, bringing theory into agreement with experiments and solving the transport
problem in Earth's core, consistent with the conventional thermal geodynamo[9]. How electron
correlations change with pressure, and how this affects material properties, will be discussed.
This work is supported by the US National Science Foundation and the ERC Advanced grant
ToMCaT.

References. [1] K. Ohta, R.E.et al. (2012): Phys. Rev. Lett, 108; [2] K. Haule, C. H. Yee, and K. Kim. (2010): Phys.
Rev. B, 81; [3] X. Sha and R. E. Cohen, J. (2011): Phys. Cond. Matt, 23, 075401; [4] N.de Koker, G.
Steinle-Neumann, and V. Vlcek. (2012): Proc Natl Acad Sci USA, 109, 4070; [5] H. Gomi, K. Ohta, K. Hirose, S.
Labrosse, R. Caracas, M. J. Verstraete, and J. W. Hernlund. (2013): Phys. Earth Planet. Int, 224, 88; [6] M. Pozzo,
C. Davies, D. Gubbins, and D. Alfe. (2012): Nature, 485, 355;[7] B. Buffett.(2012): Nature, 485, 319; [8] P. Olson.
(2013): Science, 342, 431; [9] P. Zhang, R. E. Cohen, and K. Haule. (2015): Nature, 517, 605.

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Core Neon
M. A. Bouhifd1, A.P. Jephcoat2, D. Porcelli3, S.P. Kelley4
1

Laboratoire Magmas et Volcans, Université Blaise Pascal, CNRS UMR 6524, OPGC-IRD, 5
Rue Kessler, 63038 Clermont-Ferrand Cedex, France
2
Institute for Study of the Earth's Interior, Okayama University, Yamada 827,
Misasa, Tohaku, Tottori 682-0193 Japan
3
University of Oxford, Department of Earth Sciences, Parks Road, Oxford, OX1 3AN, UK
4
Department of Environment, Earth and Ecosystems, Open University,
Milton Keynes MK7 6AA, UK
Corresponding author’s email address: andyj@okayama-u.ac.jp

Noble gases have long been the archetypal tracers of mantle processes [1]. Their inertnesscombined with an array of 23 stable isotopes has led to a wealth of mantle diagnostic studies
impinging on primordial origins and evolution, trapping history, recycling, radiogenic production,and mantle reservoir interactions. The incompatibility of noble gases has dominated the thinking
on mantle evolution coupled with outgassing to the atmosphere. The mantle likely remains thedominant source of trapped inventory to the present day. Here we consider the possibilities of acore component on noble gas budgets, and the contributions possible with the context of limited
core-mantle exchange.
The partitioning of neon between liquid silicate and molten iron-rich metal under conditionsof Earth’s early core formation to 16 GPa and ~3000K was simulated in a diamond-anvil cellunder neon-rich conditions. Ultraviolet laser ablation mass spectrometric methods were used toanalyse recovered samples. We find, as in the case of helium previously [2], that the metal phasecan contain significant, non-zero quantities of neon.
We compare the relative and absolute partitioning of Ne and He in these experiments. In thecontext of the whole Earth, the possibilities of a core signature on noble gas segregation during
accretion or an imprint on the mantle noble gas systematics as observed today are discussed.

References. [1] Hilton, D.R & Porcelli, D. (2014): Treatise in Geochemistry 2nd Edition, Vol. 3. (Turekian KK,
Holland HD, Eds.) 327-353, Oxford: Elsevier Science; [2] Bouhifd, M.A., Jephcoat, A.P., Heber, V.S., Kelley, S.P.
(2013): Nature Geosci, 6, 982-986

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Transport and Storage of Volatiles in the Mantle and Core
E. Ohtani
Department of Earth Science, Graduate school of Science
Tohoku University, Sendai, 980-8578, Japan
Corresponding author’s email address: ohtani@m.tohoku.ac.jp
Materials in the surface of the Earth including volatiles can penetrate into the deep Earththrough slab subduction. The transition zone has a water storage capacity of approximately 0.5–1
wt% due to a high water solubility in wadsleyite and ringwoodite, which are the major
constituents in the transition zone. Water has significant effects on the boundaries of the phasetransformations of the mantle minerals, and can explain some topography of the 410 and 660 km
seismic discontinuities [1]. Recent discovery of hydrous ringwoodite containing water about 1
wt. % [2] and hydrous phase Egg AlSiO3OH [3] as inclusions in diamond strongly favors
existence of the hydrous transition zone, a major water reservoir in the Earth’s interior.
We estimated the existence of the density crossover between magma and minerals at thebase of the upper mantle and the core-mantle boundary region [4, 5]. The hydrous melt formed
by dehydration melting can also be gravitationally stable at these regions [6]. Dehydration of the
wet transition zone can generate wet plumes originating at the base of the upper mantle. We
proposed a big mantle wedge model [7] caused by dehydration from the stagnant slabs, which
can explain the seismic tomographic model beneath northeast China. When subducting stabs
penetrate into the lower mantle, dehydration melting can occur also below the transition zone
[8].
We discovered a hydrous-phase AlOOH-MgSiO2(OH)2 solid solution as the reaction
product of garnet and water [9], and clarified that the end-member hydrous phase d-AlOOH isstable up to the base of the lower mantle [10]. Recently an end-member phase MgSiO2(OH)2,
named as hydrous phase H, MgSiO2(OH)2 was also reported [11, 12]. We revealed that stabilityof the end member phase H and phase d-H solid solution up to the base of the lower mantle [13,14]. The dehydration melting could occur at the base of the lower mantle providing a potential
origin of the ultra-low velocity zone at the core-mantle boundary. When this hydrous phase orhydrous magma contacts with metallic iron of the core at the core–mantle boundary, hydrogen is
likely to be dissolved into the outer core.
Measurement of the sound velocity of FeH at high pressure by using IXS (Inelastic X-ray
Scattering) revealed that the seismic velocity and density of the core can be explained byexistence of maximum 0.23(6) wt. % H in the core [15], which indicates that the core isundersaturated in hydrogen. Therefore, the core is currently a sink of hydrogen at the base of thelower mantle.
References. [1] Ohtani E. and Litasov K. (2006): Rev. Mineral. Geochemistry, vol.62, Chapter 17, 397-420; [2]Pearson, D.G. et al. (2010): Nature, 507, 7491, 221; [3] Wirth, R. et al. (2007): Earth Planet. Sci. Lett, 259, 384–
399; [4] Ohtani E. (1983): Phys. Earth Planet. Inter, 33, 12-25; [3] Ohtani E.(1985): Phys. Earth Planet. Inter.,38,
70-80; [5] Ohtani E. & Maeda, M. (2001): Earth and Planetary Science Letters, 193, 69-75; [6] Sakamaki, T. et al.
(2006): Nature, 439, 192-194; [7] D. Zhao & Ohtani E. (2009): Gondwana Research,16, Issues 3-4, 401-413; [8]Schmandt et al. (2014): Science, 344, 1265; [9] Suzuki, A.et al. (2000): Phys. Chem. Mineral, 27, 689-693; [10]Sano A. et al. (2008): Geophysical Research Letters, 35(3), L03303; [11] Tsuchiya, J.(2013): Geophys. Res. Lett, 40,
4570–4573; [12] Nishi, M. et al. (2014): Nat. Geosci, 7, 224–227; [13] Ohira I. et al. (2014): Earth and Planetary
Science Letters, 401, 12-17; [14] Ohtani E. et al. (2014): Geophysical Research Letters, 41, 23, 8283-8287; [15]Shibazaki Y. et al. (2012): Earth and Planetary Science Letters, 313-314, 79-85.

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From Star to Stone: What Really Makes an Exoplanet "Earth-like?"
C.T. Unterborn, W.R. Panero
School of Earth Sciences, The Ohio State University
Corresponding author’s email address: unterborn.1@osu.edu
Plate tectonics have operated on Earth for a majority of its lifetime. Tectonics regulates
atmospheric carbon and creates a planetary-scale water cycle, and is a primary factor in the Earthbeing habitable. While the mechanism for initiating tectonics is unknown, as we expand oursearch for habitable worlds, understanding which planetary compositions produce planets
capable of supporting long-term tectonics is of paramount importance. On Earth, thissustentation of tectonics is a function of both its structure and composition. Currently, however,
we have no method to measure the interior composition of exoplanets. In our Solar system,
though, Solar abundances for refractory elements mirror the Earth’s to within ~10%, allowing
the adoption of Solar abundances as proxies for Earth’s. It is not known, however, whether thismirroring of stellar and terrestrial planet abundances holds true for other star-planet systems
without determination of the composition of initial planetesimals via condensation sequencecalculations. Currently, all code for ascertaining these sequences are commercially available orclosed-source. We present, then, the open-source Arbitrary Composition Condensation Sequencecalculator (ArCCoS) for converting the elemental composition of a parent star to that of theplanet-building material as well as the extent of oxidation within the planetesimals.
These data allow us to constrain the likelihood for one of the main drivers for plate tectonics:
the basalt to eclogite transition subducting plates. Unlike basalt, eclogite is denser than thesurrounding mantle and thus sinks into the mantle, pulling the overlying slab with it. Without
this higher density relative to the mantle, plates stagnate at shallow depths, shutting off plate
tectonics. Using the results of ArCCoS as abundance inputs into the MELTS and HeFESTothermodynamic models, we calculate phase relations for the first basaltic crust and depleted
mantle of a terrestrial planet produced from a given stellar composition. We find that for manystellar systems, the basalt-eclogite transition does not increase plate density enough relative tothe mantle. Even should these planets initiate plate tectonics, the plate will stagnate in theshallow mantle, shutting off tectonics and produce a planet not habitable to life as we know it.
Here, we present an outline for estimating the likelihood of an extrasolar planet being “Earth-like”
and potentially habitable as well as preliminary results for various planetary systems.

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Linear Analysis on the Onset of Thermal Convection of Highly Compressible Fluids with
Variable Physical Properties: Implications for the Mantle Convection of Super-Earths
M. Kameyama
Geodynamics Research Center, Ehime University, Matsuyama, Japan
Corresponding author’s email address: kameyama@sci.ehime-u.ac.jp
A series of our linear analysis on the onset of thermal convection wasapplied to that ofhighly compressible fluids in a planar layer whosethermal conductivity and viscosity vary inspace, in order to study theinfluences of spatial variations in physical properties expected inthemantles of massive terrestrial planets.The thermal conductivity and viscosity are assumed toexponentiallydepend on depth and temperature, respectively, while the variations
inthermodynamic properties (thermal expansivity and reference density)with depth are taken to
be relevant for the super-Earths with 10 timesthe Earth's.
Our analysis demonstrated that the nature of incipient thermalconvection is strongly affectedby the interplay between the adiabaticcompression and spatial variations in physical properties of
fluids.Owing to the effects of adiabatic compression, a ``stratosphere'' canoccur in the deep
mantles of super-Earths, where a vertical motion isinsignificant.An emergence of ''stratosphere''is greatly enhanced by the increase inthermal conductivity with depth, while it is suppressed by
the decreasein thermal expansivity with depth.In addition, by the interplay between the static
stability and strongtemperature-dependence in viscosity, convection cells tend to beconfined in
narrow regions around the ''tropopause'' at the interfacebetween the ''stratosphere'' of stablestratification and the''troposphere'' of unstable stratification.
We also found that, depending on the variations in physical properties,two kinds of stagnant
regions can separately develop in the fluid layer.One is well-known ``stagnant-lids'' of cold andhighly viscous fluids,and the other is ``basal stagnant regions'' of hot and less viscousfluids.The
occurrence of ``basal stagnant regions'' may imply that convectingmotions can be insignificant in
the lowermost part of the mantles ofmassive super-Earths, even in the absence of strong
depth-dependence inviscosity.

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Melting of Sahara 97072 Meteorite (EH3 Chondrite) at 12 GPa and Variable Temperatures
W. Du1,2, T. Irifune1,2
1

Geodynamics Research Center, Ehime University
Earth-Life Science Institute, Tokyo Institute of Technology
Corresponding author’s email address: wei_du@sci.ehime-u.ac.jp
2

The accretion and early differentiation of the Earth is the starting point of earth
history.Because of their isotopically identical to the Earth, enstatitechondrites(E-chondrite) havebeen proposed as a model for the chemical composition of the bulk Earth [1, 2].However, themost recent study on silicon isotope by Fitoussi and Bourdon (2012)[3] argued that to get
consistent with the isotopic composition of bulk silicate Earth, the Earth’s core need to containas much as 28 wt% Si, which is then not consistent with the density deficit deduced from seismic
velocities.Start from an estimate of the bulk earth composition to evaluate the conditions ofcore–mantle differentiation by simple melting experiments at high temperature and relatively
high pressure could be an alternative strategy to evaluate the proposed models for the Earth’s
formationand its early differentiation.
In this study, we present the first serial of melting experiments on Sahara 97072 meteorite,
an EH3 chondrite with least metamorphosed [4] at relatively high pressure (12 GPa) anddifferent temperatures (1000-2000°C), to compare the liquid silicate composition with the bulk
mantle compositionthat is predicted from the proposed models, and ultimately to test the
hypothesis of the building block of the Earth has similar composition as enstatitechondrite.
Experiments at 12GPa and different temperatures were carried with Kawai-type multi-anvil
devices at GRC, Ehime University. With increasing temperature from 1500 to 1900°C, theresidual crystalline phase assemblage changes from opx+garnet+olivine, garnet+olivine, and toolivine. The melting temperature of Sahara 97072 meteorite at 12 GPa is almost the same as thereported melting relation of Allende meteorite[5]. Olivine is the liquidus phase for Sahara 97072
meteorite at 12 GPa; silicate solidus is about 1700°C and silicate liquidus is 1900°C,
wheresilicate liquid coexisting with metallic liquid. At temperature higher than 1800°C, olivine
started to melt to periclase + liquid phase. Magnesiowüstitewas detected at the reaction zone
between metallic liquid and silicate liquid, which could be caused by the losing of sulfur from
sulfide liquid. Ni and Co content in the melt metallic phases increase with temperature.
Solidification of metallic phase shows exsolution of a more nickel rich and iron poor metallic
phase coexisting with iron-nickel sulfide. The losing of S from metallic liquid phase to either
silicate liquid or to the air will cause large changes on the partitioning of siderophile elements
between the metallic phases and the silicate phases.

References:[1] Javoy, M. (1995): GRL, 22, 2219-2222; [2] Javoy, M. et al. (2010): Earth and Planetary Science
Letters, 293, 259-268; [3] Fitoussi, C. and Bourdon, B. (2012): Science,335, 1477-1480; [4] Lehner, S.W. et al.
(2011): Lunar and Planetary Science Conference, 42, 1430; [5] Agee, CB et al. (1995): Journal of GeophysicalResearch: Solid Earth, 100, 17725-17740.

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Effective Temperature Condition in the Separation Process of the Core and Mantle
H. Ichikawa1,2, J. Hernlund2, S. Labrosse3, M. Kameyama1
1

Geodynamics research Center, Ehime University
Earth-Life Science Institute, Tokyo Institute of Technology
3
Ecole normale supérieure de Lyon
Corresponding author’s email address: h-ichikawa@sci.ehime-u.ac.jp
2

It has been long known that the formation of the core transforms gravitational energy into
heat and is able to heat up the whole Earth by about 2000 K. However, the distribution of thisenergy within the Earth is still debated and depends on the core formation process considered.
Iron rain in the surface magma ocean is supposed to be the first mechanism of separation forlarge planets, iron then coalesces to form a pond at the base of the magma ocean. In this process,equilibrium between metal and silicate is achieved within several seconds [1].
Experimental studies of metal-silicate partition coefficient show that pressure-temperature
conditions for metal-silicate equilibrium are far beyond the liquidus or solidus temperature forseveral hundred kelvin [e.g. 2]. However, because equilibration was considered to occur in at thesurface of metal pond at the silicate solidus, such high temperature equilibration was rejected as
implausible. Instead, lower temperature equilibration with variable oxygen fugacity was
proposed as an alternative, although the plausibility of the physical mechanisms invoked in this
scenario is also questionable.
In this study, we model iron rain and heating of the magma by viscous dissipation to
calculate the effective pressure-temperature conditions for partitioning in this scenario based onparameterizations derived from direct numerical simulation results of cm-scale emulsion ofliquid iron in liquid silicates. We have found effective temperature is much higher than themelting temperature of silicate due to the release of gravitational potential energy. We have also
found that the magma ocean depth of 1500-2500 km is consistent with estimated compositions of
the core and the mantle.

References. [1] Ichikawa, H., Labrosse, S., Kurita, K. (2010): JGR, 115, B01404, doi:10.1029/2009JB006427; [2]Wade, J. & Wood, B. (2005): EPSL, 236, 78-95.

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Effect of a Stratified Basal Magma Ocean on the Geodynamo
M. Laneuville1, J. Hernlund1, S. Labrosse2, N. Guttenberg1
1

2

Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo, Japan
Département des Sciences de la Terre, Ecole Normale Supérieure, Lyon, France
Corresponding author’s email address: mlaneuville@elsi.jp

Earth’s magnetic field is thought to be sustained by dynamo action in a convecting metallic
outer core since at least 3.45 Ga [1]. Convection induces an isentropic temperature gradient thatdrains 13±3 TW of heat from the core by thermal conduction [2-4], and suggests that Earth’s
core has cooled by 1,000 K or more since Earth’s formation [4,5]. However, models of Earth’s
initial thermal evolution following a giant-impact predict rapid cooling to the mantle melting
temperature (e.g., [6]).
In order to understand how the core could have retained enough heat to explain the age ofthe geodynamo, we relax a key assumption of the basal magma ocean model of [7] to allow for
the possibility that the magma is stably stratified. Recent giant impact simulations suggest
extensive core-mantle mixing [8], which could have produced such a large stratified magma
layer at the core-mantle boundary. Turbulent metal-silicate mixing in a magma ocean could also
lead to a stable strafication [9].
In the presence of a stable density gradient, heat transfer through the basal magma ocean
occurs through conduction and therefore delays heat loss from the core. Partitioning of iron in
the liquid phase upon crystallization changes the density profile and triggers convection in theupper part of the basal magma ocean. Our hypothesis suggests that early core cooling is
dominated by the timescale on which the stratification is eroded, and a more efficient corecooling (i.e, the amount of heat extracted from the core is closer to what is actually recquired todrive the geodynamo).

References. [1] Tarduno, J. et al. (2010): Science, 327, 1238-1240;[2] de Koker, N. et al. (2012): Proc. Natl. Acad.
Sci, 190, 4070-4073; [3] Pozzo, M. et al. (2012): Nature, 485, 355-358; [4] Gomi, H. et al. (2013): Phys. Earth
Planet. Inter, 224, 88-103; [5] Labrosse, S. (2015): Phys. Earth Planet.Inter, in press; [6] Solomatov, V.S. (2007):In Treatise on Geophysics,9, 91-120; [7] Labrosse, S. et al. (2007): Nature, 450, 866–869; [8] Saitoh, T. and Makino,
J. (2013): Astrophys. J, 768, 44; [9] Deguen et al. (2011): Earth Planet. Sci. Lett, 310, 303-313.

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Major Element Composition of the Early Enriched Reservoir: Constraints from142
Nd/144Nd Isotope Systematics in the Early Earth and High-pressure
Melting Experiments of Primitive Peridotite
N. Kondo1, T. Yoshino2, K.N. Matsukage3, T. Kogiso4
1

Gradudate School of Human and Environmental Studies, Kyoto University
2
Institute for Study of the Earth’s Interior, Okayama University
3
Tokyo Institute of Technology
Corresponding author’s email address: kondo.nozomi.75x@st.kyoto-u.ac.jp

Present Accessible Silicate Earth (ASE) has significantly higher 142Nd/144Nd than chondrites[1]. In order to compensate the difference between ASE and chondrites, there should have been
low 142Nd/144Nd reservoir, which formed as melt in the early Earth (Early Enriched Reservoir,
EER). The major element composition of EER has been still unclear, though it is crucial toestimate its chemical and physical properties, and essential to understand the origin and destinyof EER, which affects present composition of the Earth. In order to determine the major element
composition of EER, we estimated the age and pressure-temperature condition of EER formationthat can explain the Nd isotopic characteristics of EER, on the basis of the Sm-Nd partitioning
and its dependence on pressure, temperature, and melting phase relation. We determined the
major element composition of EER at the estimated pressure-temperature condition, withhigh-pressure melting experiments of the primitive peridotite, and calculated density of EER.
The EER was estimated to have formed within 33.5 Myr after the solar system formation
and at near-solidus temperature at a shallow upper mantle pressure. The result of ourexperiments and previous studies indicate that the near-solidus melt is Fe-komatiitic at 7 GPa,and picritic to basaltic at pressure less than 3 GPa. The estimated density of the near-solidus melt
is smaller than that of the primitive peridotite, suggesting that EER ascended in the mantle, andformed crust. Because the mantle potential temperature would have been very high in the
Hadean, EER should have formed at high pressure, and therefore its composition would havebeen Fe-rich komatiitic to picritic. Because the EER formation precedes to the Moon forming
last giant impact, EER, the Hadean komatiitic-picritic crust, was probably spattered from the
Earth before or at the last giant impact. Thus EER has been lost, leaving the present Earthnon-chondritic.

References. [1] Boyet, M & Carlson, R. W. (2005): Science, 309, 576-581.

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Ab initio Electrical Resistivity of hcp Iron at Earth’s inner Core Conditions
H. Dekura
Geodynamics Research Center, Ehime University
Corresponding author’s email address: dekura.haruhiko.mf@ehime-u.ac.jp
Electrical resistivity of minerals at high-pressure and temperature is one of the most
unconstrained properties in deep Earth science. Determination of the electrical resistivity of iron,
as a major component of the Earth’s core, is essential to discuss its dynamics. Direct
experimental determination is known extremely difficult. On the other hand, recent development
in computational physics is now accessible to calculations of the electron transport property ateven multi-megabar and thousands Kelvin. We have been developing a technique to computeelectron-phonon interaction and electrical resistivity of minerals based on the density-functional
perturbation theory with the Bolthzmann electron transport theory. In this presentation, I willshow the detailed information of the method and show a preliminary result of resistivity of hcp
Fe calculated at the conditions corresponding to center of the Earth.

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Hugoniot and Temperature Measurements of H2O up to 260 GPa
Under Laser-driven Shock Loading
T. Kimura1, N. Ozaki2,3, T. Sano4, T. Okuchi5, T. Sano2, K. Shimizu6, K. Miyanishi2,
T. Terai2, T. Kakeshita2, Y. Sakawa4, R. Kodama2,3
1

Geodynamics Research Center, Ehime University
Graduate School of Engineering, Osaka University
3
Photon Pioneers Center, Osaka University
4
Institute of Laser Engineering, Osaka University
5
Institute for Study of the Earth’s Interior, Okayama University
6
KYOKUGEN Center for Science and Technology under Extreme Conditions, Osaka University
Corresponding author’s email address: t_kimura@sci.ehime-u.ac.jp
2

Pressure, density, and temperature data for H2O were obtained up to 260 GPa by using
laser-driven shock compression technique. The diamond cell applied for the laser shock
experiments was used as the sample container in order to achieve temperature conditions lower
than the principal Hugoniot states. This shock technique combined with the high-pressure cell
can be used for an assessment the equation of state models because it is possible to compare thestates under the conditions that the contrast between the models clearly appears. Our P-r-T data
are in totally agreement with those of the model based on quantum molecular dynamics
calculations. These facts indicate that this model is adopted as the standard for modeling interior
structures of Neptune, Uranus, and exoplanets in the liquid phase in the mult-Mbar range[1].

References. [1] Kimura, T. et al. (2015): J. Chem. Phys., 142, 164504.

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High-pressure in situ X-ray Laminography Using Diamond Anvil Cell
R. Nomura1, K. Uesugi2
1

Earth-Life Science Institute, Tokyo Institute of Technology, 2JASRI/SPring-8
Corresponding author’s email address: nomura.r.ab@m.titech.ac.jp

Diamond anvil cell (DAC) is a powerful tool to reproduce high pressure (P) and hightemperature (T) conditions corresponding to the deep Earth interiors in a laboratory [e.g. 1].
Various types of measurements such as in situ high P-T spectroscopies and ex situ chemical
analysis have been conducted using DAC to understand the physics and chemistry of the Earthmaterials.
Among them, 3D visualization and textural/chemical characterization of the internal
structure of the sample at high P-T is of great importance. In situ high-P x-ray computed
tomography (CT) has been developed by transmitting x-rays through a sample and a light metal
gasket (e.g. Be) between diamond anvils. Recently, the dihedral angle of molten iron between
bridgmanite was investigated at high-pressure by using laser-heated DAC combining with x-ray
computed tomography (CT) with profound implications for the physical process of the Earth’s
core-mantle separation [2]. On the other hand, Tsuchiyama et al. (2013) [3] developed “chemical
imaging” techniques known as analytical dual-energy microtomography in which the two x-ray
energies below and above the absorption energy of a targeted element are used for imaging.
Although this technique is powerful for chemical purpose, an application to in situ high P-Tremains technically challenging because typical Earth’s major elements have an absorption edgein near soft x-ray energy, in which even Be gasket absorbs the incident x-rays crucially.
X-ray laminography, which has an inclined rotational axis to x-ray, is a suitable technique toapply for diamond anvil cell because x-ray can avoid the gasket to obtain projection images. This
technique is generally used to obtain the internal structures of a laterally-extended objects inthree dimensions. Although x-ray laminography loses the quantitative information of linear
attenuation coefficients, it is still useful for qualitative chemical analysis by combining dual
energy x-ray techniques.
In this presentation, we will show our recent developments on in situhigh pressure x-ray
laminography techniques by using a diamond anvil cell.

References. [1] Tateno, S. et al. (2010): Science, 330, 359-361; [2] Shi, C. (2013): Nature Geoscience, 6, 971-975;[3] Tsuchiyama, A. et al. (2013): Geochim. Cosmochim. Acta, 116, 5-16.

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Phase Relations of FeH at Earth’s Core Pressure
C. Kato1, K. Ohta1, K. Hirose2,3, Y. Ohishi4
1

2

Department of Earth and Planetary Sciences, Tokyo Tech
Earth-Life Science Institute, Tokyo Institute of Technology, 3JAMSTEC, 4JASRI
Corresponding author’s email address: kato.c.ab@m.titech.ac.jp

Hydrogen is one of the plausible candidates of light element(s) in the Earth’s core. Previous
studies suggested that hydrogen preferentially partitioned into liquid metallic iron core as FeHx
in the magma ocean of the primordial Earth. [e.g., 1, 2]. In-situ X-ray diffraction experiments
revealed that FeHx with double-hexagonal close packed (dhcp) structure formed at 3.5 GPa andthe structure did not change up to at least 80 GPa [3,4]. Energetic calculations indicate thestructural transition of dhcp to hexagonal close packed (hcp), and hcp to face-centered cubic (fcc)
structure at the Earth’s lower mantle pressure [5]. However, the suggested phase transitions of
FeHx have not been verified by experiments, and therefore the crystal structure of FeHx undercore pressures is still an open question.
We examined the phase relations of FeHx at high pressures and high temperatures in alaser-heated diamond-anvil cell based on synchrotron X-ray diffraction measurements at
BL10XU, SPring-8. The results show that dhcp-FeHx disappeared and hcp-FeHx formed at ~60
GPa, and hcp-FeHx underwent transformation into fcc-FeHx at ~70 GPa. We also obtained thepressure-volume (P-V) data of fcc-FeHx at 26 to 137 GPa and 300 K. The compressivity showeda discontinuous change at ~70 GPa, which may be induced by a magnetic transition of fcc-FeHx,
as indicated by the theoretical calculation [5]. Based on our experimental results, we argue that alikely crystal structure of FeHx at least at the Earth’s topmost core conditions is fcc structure
rather than dhcp and hcp.

References. [1] Fukai. (1984): Nature, 208, 174-175; [2] Okuchi et al. (1997): Science, 278, 1761-1784; [3] Badding
et al. (1991): Science, 253, 421–424. [4] Hirao et al. (2004): GRL, 31, L06616; [5] Isaev et al. (2007): PNAS, 104,
9268-9171.

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The Eutectic Liquid Composition in the Fe-Fe3S Binary System at the Core Pressure Range
Y. Mori1, S. Tateno2, K. Hirose3, G. Morard4, Y. Ohishi51

Department of Earth and Planetary Sciences, Tokyo Institute of Technology
2Institute for Study of the Earth's Interior, Okayama University
3
Earth-Life Science Institute, Tokyo Institute of Technology
4
IMPMC, Universite Pierre-et-Marie-Curie
5
Japan Synchrotron Radiation Research Institute
Corresponding author’s email address: mori.y.ah@m.titech.ac.jp

Sulfur is considered to be an important component in the Earth's core because it is depleted
in the crust and mantle compared to other volatile elements and often included in iron meteorites.
Here we examine the liquidus phase relations in the Fe-Fe3S binary system between 38 and 138
GPa based on characterization of a sample recovered from a melting experiment at high pressure
and temperature in a laser-heated diamond-anvil cell. Both Fe-8wt.%S and Fe-14wt.%S samples
were employed as starting materials, which were homogeneous mixtures of fine-grain Fe andFeS (<1 µm) prepared by induction melting and rapid quenching technique [1]. We used afocused ion beam (FIB) equipped with energy dispersive X-ray spectrometry (EDS) for texturaland chemical characterizations of recovered samples. The samples exhibited a melting texture
with quenched liquid alloy at the hottest part and solid Fe or Fe3S at its outside. In a couple ofsamples, the quenched liquid was in direct contact with solid Fe3S, and solid Fe was also present
right next to Fe3S, suggesting that the composition of such liquid is close to a eutectic
composition (~12 wt.% S at 66 GPa and ~10 wt.% S at 138 GPa). Indeed, this interpretation isconsistent with the results of other experiments obtained in this study. Our data demonstrate thatthe eutectic liquid composition in the Fe-Fe3S binary system decreases its sulfur concentration
with increasing pressure, which is in agreement with previous studies [2,3]. The sulfur content in
the eutectic liquid composition may be less than 10 wt.% at the inner core boundary pressure.
The recent shock-wave study by Huang et al. [2013 GRL] suggested 10 wt.% S in the outer core,
but the present study indicates that such liquid alloy with 10 wt.% S crystalizes the B2 phase of
Fe-S alloy and thus does not support the sulfur-rich outer core.

References. [1] Morard et al. (2011): PCM, 38, 767-776; [2] Morard et al. (2008): EPSL, 272, 620-626; [3] Kamada
et al. (2012): EPSL, 359, 26-33.

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Some Thermodynamic Properties of Larnite (β-Ca2SiO4)
Constrained by High T/P Experiment and/or Theoretical Simulation
Z.H. Xiong1, X. Liu2, S.R. Shieh3,
1

Geodynamics Research Center, Ehime University
School of Earth and Space Science, Peking University
3
Department of Earth Sciences, University of Western Ontario
Corresponding author’s email address: xiong.zhihua.gf@ehime-u.ac.jp
2

Natural larnite (Lrn; β-Ca2SiO4; space group P21/n with Z = 4) was firstly reported in the
Larne district of Great Britain [1], and soon documented on the island of Muck in Scotland[2]and the Tokatoka region in New Zealand [3]. It usually locates in the contact zone between an
igneous rock like dolerite or andesite, and a calcitic rock such as chalk or limestone [1, 3]. This
conventional field occurrence of Lrn was recently supplemented with another completely
different appearance, tiny mineral inclusions, usually coexisting with the walstromite-structured
CaSiO3 (Wal) and titanite-structured CaSi2O5 (Ttn), in diamonds possibly originating from thelower mantle [4, 5, 6]. This new appearance strongly argues that some portions of the deep
interior of the Earth are significantly Ca-richer than the normal pyrolitic mantle [7].
In study, pure larnite (β-Ca2SiO4; Lrn) was synthesized at 6 GPa and 1473 K for 6 hours byusing a cubic press, its thermal expansivity was investigated up to 923K by using an X-ray
powder diffraction technique (ambient P), and its compressibility was investigated up to ~16
GPa by using a diamond-anvil cell coupled with synchrotron X-ray radiation (ambient T). Its
volumetric thermal expansion coefficient (αV) and isothermal bulk modulus (KT) wereconstrained as αV = 4.24(4)×10-5/K and KT = 103(2) GPa (the first pressure derivative K T'
obtained as 5.4(4)), respectively. Its compressibility was further studied with the CASTEP codeusing density functional theory and planewave pseudopotential technique. We obtained the KT
values as 123(3) GPa (LDA; high boundary) and 92(2) GPa (GGA; low boundary), with thevalues of the K T' as 4.4(9) and 4.9(5), respectively.The phonon dispersions and vibrational
density of states (VDoS) of Lrn were simulated using density functional perturbation theory, andthe VDoS was combined with a quasi-harmonic approximation to compute the isobaric heat0capacity (CP) and vibrational entropy ( S 298), yielding CP = 212.1(1) – 9.69(5)×102T-0.5 –
04.1(3)×106T-2 + 5.20(7)×108T-3 J mol-1 K-1 for the T range of ~298-1000 K and S 298= 129.8(13)-1-1J mol K . In addition, the microscopic and macroscopic thermal Grüneisen parameters of Lrn
at 298 K were calculated to be 0.75(6) and 1.80(4), respectively.

References. [1] Tilley, C.E. (1929): Mineral Mag, 22, 77-86; [2] Tilley, C.E. (1947): B Com Geol Finlande, 140,
97-106; [3] Mason, B. (1957): Am Mineral, 42, 379-392; [4] Joswig, W., Stachel, T.H., Harris, J.W., Baur, W.H.
and Brey, G.P. (1999): Earth Planetary Sci Lett, 173, 1-6; [5] Nasdala, L., Brenker, F.E., Glinnemann, J.,
Hofmeister, W., Gasparik, T., Harris, J.W., Stachel, T. and Reese, I. (2003): Eur J Mineral, 15, 931-935; [6]Brenker, F.E., Vincze, L., Vekemans, B., Nasdala, L., Stachel, T., Vollmer, C,. Kersten, M., Somogyi, A., Adams,F., Joswig, W. and Harris, J.W. (2005): Earth Planetary Sci Lett, 236, 579-587; [7] Ringwood, A.E. (1975):
McGraw-Hill, New York.

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The Lower Mantle: A Seismological Perspective
B.L.N. Kennett
Research School of Earth Sciences, The Australian National University
Corresponding author’s email address: Brian.Kennett@anu.edu.au
The structure of the lower mantle appeared to be simple when summarized by 1-D earthmodels, but has become progressively more complex as we have learnt more about the 3-D
structure of the Earth. The point at which one leaves the mantle transition zone and enters thelower mantle is not well defined, but can be conveniently taken as the depth at which majorite
garnet is extinguished (around 850 km deep) where viscosity reaches a high value. Away fromthe major sources of colder material in former subduction zones, the levels of seismic
heterogeneity are modest though stronger in shear wavespeed than bulk-sound speed. Suchheterogeneity increases significantly below 2100 km depth, though this is not what is expectedfrom the effect of pressure. The increase in wavespeed variability occurs well before any
influence from post-perovskite material could be expected.
Different styles of investigation give very consistent pictures of the major features in lower
mantle structure and support the presence of zones of lower wavespeed material rising well into
the middle mantle. It is tempting to regard wavespeed reduction as due to temperature, but therelative behavior of the bulk and shear moduli suggests that chemical heterogeneity cannot beignored. Recent work using full-waveform inversion of long-period seismograms suggests thatsome lower wavespeed material may be organized into relatively narrow features beneathrecognized hot spots - are these the elusive plumes?

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Persistence of Strong Silica-Enriched Domains in the Earth's Lower Mantle
J.W. Hernlund1, C. Houser1, M.D. Ballmer1,2,
R. Wentzcovitch1,3, K. Hirose1
1

Earth-Life Science Institute, Tokyo Institute of Technology, Meguro, Tokyo, Japan
2
Institute of Geophysics, ETH Zurich, Zurich, Switzerland
3
Chemical Engineering and Materials Science Department, University of Minnesota

The chemical composition of the Earth’s lower mantle, the largest region of our planet,
ispoorly constrained. While some geochemical observations suggest a lower mantle bulk
com-position that differs from the shallow mantle, geophysical evidence suggests that wholemantle convection and associated mixing should have largely erased any major differences.
Herewe use numerical models of mantle convection to show that large silica-enriched domains
inthe lower mantle are stable against mixing owing to a modest increase in density andhigherviscosity that results from greater abundance of the strong (Mg,Fe)SiO3-bridgmanite
mineral phase. The style of mantle convection in such circumstances exhibits strong coresofbridgmanite enriched ancient mantle structures (BEAMS) separated by conduits of
weakersilica-depleted rocks that circulate between the shallow and deep mantle. This patternofconvection is stable over timescales much longer than the age of the Earth, even for
relativelymodest viscosity and density increases in BEAMS material, thus permitting significant
com-position differences between the deeper and shallower mantle to be compatible with whole1
mantle convection. Our models exhibit strong memory effects upon lower mantle
convectiveplanform, stabilizing the location of upwelling and downwelling flows through the
deep man-tle over billions of years. The BEAMS model may help to reconcile differences
between thecomposition of the shallow mantle and that of the Sun and chondritic meteorites.

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Discovery of New Iron Oxide Fe7O9 and Its Solid Solution, (Mg,Fe2+)3Fe3+4O9
R. Sinmyo1,*, E. Bykova1, SV. Ovsyannikov1, C. McCammon1, I. Kupenko2,
L. Ismailova1, L. Dubrovinsky1
1

2

Bayerisches Geoinstitut, Universitaet Bayreuth
Europian Synchrotron Radiation Facility, *Now at Earth-Life Science InstituteTokyo Institute of Technology
Corresponding author’s email address: ryosuke.sinmyo@elsi.jp

Iron oxides are fundamentally important compounds for the terrestrial planets. The stability
and properties of iron oxides are essential information to understand the evolution of redox stateof the Earth’s mantle and surface. Here we report new high-pressure polymorphs of iron oxide
Fe7O9 (Fe3+/Fe2+ = 4/3) and its Fe2+-Mg solid solution (Mg,Fe2+)3Fe3+4O9 that can be recoveredat ambient conditions. We synthesized single crystals of the both compounds at about 24-26 GPausing a multi-anvil press. Single crystal X-ray diffraction (XRD) studies showed that the crystal
structures of both Fe7O9 and (Mg,Fe2+)3Fe3+4O9 have monoclinic C2/m space groups, that differ
from any other known lattices of iron oxides. Mössbauer spectra are in agreement with the
crystal structure refined from single crystal XRD. This newly found Fe7O9 polymorph suggeststhat iron oxides may have more variable mixed valence state under high-pressure condition thanpreviously thought. Based on analogy with Fe2+1+nFe3+2O4+n group, a Fe2+3±nFe3+4O9±n group
might be also stable at certain high pressures and temperatures and oxygen fugacity. Some
Fe3+-rich phase found in diamond inclusion may be a back-transformed high-pressure polymorphof these iron oxides. The phase relation of such new iron-oxide group may provide a new insightfor redox state of the Earth’s mantle.

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Helium Diffusion in Mantle Minerals from First Principles
John Brodholt (UCL)
We have used ab initio DFT methods to calculate the diffusion coefficients of He in olivine,
perovskite and post-perovskite under lower mantle conditions. The diffusion coefficients were
calculated using the nudged-elastic band method to find the minimum energy pathway and themigration enthalpy. The harmonic Vinyard theory was used to calculate the migration entropy
and attempt frequency. In perovskite and post-perovskite, He diffusion is so fast that we canalso estimate the diffusion coefficient directly in an ab initio molecular dynamics simulation.
The two methods agree well with each other.
The diffusion coefficients of He in olivine agree extremely well with existing experiments
and is fast. For instance, in the upper mantle He can diffuse between 1 and 50 meters in 1 million
years. Interestingly, diffusion in perovksite is even faster (perhaps by two orders of magnitude)
and in the deepest Earth, diffusion coefficients are sufficiently high so as to be able tohomogenise reservoirs of up to 50 km over the age of the Earth. The source of high 3/4He
reservoirs must, therefore, be larger than this if they are to exist for the age of the Earth.
Moreover, larger reservoirs of high 3/4He will essentially pollute the mantle around them andpotentially some high 3/4He signals at the surface will be decoupled from other “hotspot”-likeisotopic signals.
Finally, our results suggest that He solubility in the lower mantle is much smaller than in theupper mantle. This is supported by some experiments in the multi-anvil we have performed.

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Modes of Slab Behavior: from the Transition Zone to the Mid-Lower Mantle
C.R. Bina1, H. Čížková2
1
Department of Earth and Planetary Sciences, Northwestern University, U.S.A
2
Faculty of Mathematics and Physics, Charles University in Prague, Czech Republic
Corresponding author’s email address: craig@earth.northwestern.edu
Subducting slabs may exhibit buckling instabilities and consequent folding behavior in the
mantle transition zone, accompanied by temporal variations in dip angle, plate velocity, andtrench retreat. Governing parameters include both viscous (rheological) and buoyancy(thermo-petrological) forces. Numerical experiments suggest that many parameter sets lead toslab deflection at the base of the transition zone, typically accompanied by quasi-periodic
oscillations in largely anticorrelated plate and rollback velocities, resulting in undulating
stagnant slabs as buckle folds accumulate subhorizontally atop the lower mantle. Slabpetrology – of mantle phase transitions and hydrated crust – is a dominant factor in this process[1]. For terrestrial model parameters, trench retreat is common and trench advance quite rare,
due to rheological and ridge-push effects. Global plate-motion studies indicate that trenchadvance is rare on Earth, too, being largely restricted to the Marianas-Izu-Bonin arc. Dynamical
models based on the unusual double-subduction geometry of the Philippine Sea region do yieldpersistent trench advance [2].
Imaging of buckled stagnant slabs is complicated by smoothing effects inherent in seismic
tomography, but velocity structures for petrologically layered slabs, spatially low-pass filteredfor comparison with tomography of corresponding resolution, yield a better fit to VP anomalies
from stagnant slab material beneath northeast China for undulating (vs. flat-lying) slabs [3].
Earthquake hypocentral distributions and focal mechanisms (especially below 660 km) also
provide insights into slab buckling in regions of slab stagnation [4], and these can be compared
to stress fields computed from our dynamical models.
A combination of driving forces governs slab stagnation. Buoyancy arising from thermal
perturbation of equilibrium phase transitions contributes to slab bending and may partly control
depth of stagnation [5]. Additional buoyancy from possible metastable persistence of olivine or
pyroxene phases may enhance slab stagnation, and temporal decay of such metastability bythermal equilibration may lead to slab foundering [5, 6, 7, 8, 9]. Complexities in mantle
viscosity structure, associated with mineralogical transitions, may also contribute to slab
stagnation [1, 10].
Subsequent descent of buckled slab material into the lower mantle may occur in a variety
of ways: drawn downward from the distal (relative to the trench) edge, from the proximal edge,or from somewhere in between [11], or by bulk foundering of the entire megalith-like mass.
Mode selection appears to be governed by factors such as rheological structure and trenchmotion.
Presence of foundered slab material is likely indicated by seismic scatterers observed in the
mid-lower mantle [12]. Proposed origins of such scatterers include: structural transitions inrelict silica phases [13], electronic spin transitions in hydrous ferromagnesian silicates [14], andelectronic spin transitions in alkalic hexagonal aluminous phases [15], all occurring primarily
within subducted crustal material.

References. [1] Čížková, H. & Bina, C.R. (2013): EPSL, 379, 95-103; [2] Čížková, H. & Bina, C.R. (2015): EPSL,
430, 408-415; [3] Zhang, Y. et al. (2013): GGG, 14, 1182-1199; [4] Fukao, Y., et al. (2014): JpGU abst., SIT03-12;[5] Bina, C.R. & Kawakatsu, H. (2010): PEPI, 183, 330-340; [6] Bina, C.R. (2013): Nature Geosci, 6, 335-336; [7]Bina, C.R. (2013): IWMMLD abst., 39; [8] Agrusta, R., van Hunen, J., Goes, S. (2014): GRL, 41, 8800-8808; [9]King, S.J., Frost, D.J., Rubie, D.C. (2015): Geology, 43, 231-234; [10] Marquardt, H. & Miyagi, L. (2015): Nature
Geosci, 8, 311-314; [11] Christensen, U.R. (1996): EPSL, 140, 27-39; [12] Kaneshima, S. & Helffrich, G. (2010):
PEPI, 183, 91-103; [13] Bina, C.R. (2010): PEPI, 183, 110-114; [14] Chang, Y.-Y. et al. (2013): EPSL, 382, 1-9;[15] Wu, Y. et al. (2014): AGU abst., MR24-04.
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Multiscale Seismic Tomography and Mantle Dynamics
D.P. Zhao
Department of Geophysics, Tohoku University, Sendai, Japan
Corresponding author’s email address: zhao@aob.gp.tohoku.ac.jp
We determined a new global P-wave tomography model using a flexible-gridparameteri-zation, 3-D ray tracing and five kinds of mantle phases (P, pP, PP, PcP & Pdiff) [1, 2].
This new model better reveals the mantle structure under the polar regions than the previous
models. The subducting slabs are generally imaged clearly as high-velocity (high-V) zones. The
young slabs are still subducting in the upper mantle and the mantle transition zone (MTZ),
whereas the old and ancient slabs are either stagnant in the MTZ or have subducted down to thelower mantle, even reaching the core-mantle boundary. Low-velocity (low-V) anomalies are
generally revealed in the mantle under the hotspot regions. It seems that a variety of mantle
upwelling (plumes) exist. Some strong plumes are visible in the whole mantle under the
long-living hotspots, whereas weak plumes are visible in only some depth range under the minor
hotspots. Beneath the intraplate volcanoes in East Asia, Bering Sea and West Alaska, significant
low-V anomalies are revealed in the upper mantle, which may reflect hot and wet upwellingassociated with corner flows in the Big Mantle Wedge (BMW) above the stagnant Pacific slab in
the MTZ and perhaps deep slab dehydration as well. The subduction-triggered magmatism in the
BMW may be a new class of mantle plumes.
Our high-resolution regional tomography revealed more details on the origin of theintraplate volcanism in East Asia [2-4]. The active Tengchong volcano in Southwest China isunderlain by a prominent low-V anomaly in the shallow mantle, which may be caused by the
subduction and dehydration of the Burma microplate plate (or the Indian plate). The Hainan
volcano is underlain by a plume-like low-V anomaly that extends down to at least 1000 km
depth and seems to be related to the deep subductions of the Burma microplate (or the Indian
plate) in the west and the Philippine Sea plate in the east. Prominent low-V anomalies aredetected beneath the Changbai, Longgang and Xianjindao volcanoes in Northeast Asia, which
may be related to the rollback of the subducting Pacific slab as well as convective circulation
processes in the BMW above the stagnant slab. The origin of the Wudalianchi volcano in
Northeast China seems associated with the upwelling of asthenospheric materials caused by
subduction-induced lithospheric delamination.
We also determined P-wave anisotropic tomography of the Western Pacific subduction
zones and SE Asia [4, 5]. The P-wave azimuthal anisotropy exghibits a fast-velocity direction(FVD) of NE-SW (trench parallel) in the subducting Philippine Sea slab beneath the Ryukyu arc,
which is consistent with the spreading direction of the West Philippine Basin during its initial
opening stage, suggesting that it may reflect a fossil anisotropy. A striking variation of the FVD
with depth is revealed in the subducting Pacific slab beneath the Northeast Japan arc, which may
be caused by slab dehydration that changed elastic properties of the slab with depth. The FVD in
the mantle wedge beneath the Northeast Japan and Ryukyu arcs is trench normal, which reflects
subduction-induced convection. Beneath the Kuril and Izu-Bonin arcs where oblique subduction
occurs, the FVD in the mantle wedge is nearly normal to the moving direction of the downgoing
Pacific plate, suggesting that the oblique subduction together with the complex slab morphology
have disturbed the mantle flow there.
References. [1] Zhao, D. et al. (2013): Gondwana Res, 23, 595-616; [2] Zhao, D. (2015): Multiscale Seismic
Tomography. Springer, 304; [3] Wei, W. et al. (2012): J. Asian Earth Sci, 60, 88-103; [4] Wei, W. et al. (2015): J.
Geophys.Res, 120, 1642-1666; [5] Huang, Z. et al. (2015): J. Geophys.Res, 120, 5154-5174.
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Three-dimensional Analysis of Pore Effect on Composite Elasticity
by Means of Finite Element Method
A. Yoneda
ISEI, OkayamaUniversity
A three-dimensional buffer-layer finite element method (FEM) model was developed toinvestigate the porosity effect on macroscopic elasticity. Using the three-dimensionalmodel, theeffect of pores on bulkeffective elastic properties were systematically analyzed by changing thedegree of porosity, the aspect ratio of the ellipsoidal pore, and the elasticity of the material. The
present results in 3D space were compared with the previous ones in 2D space. Derivatives ofnormalized elastic stiffness constants with respect to needle-type porosity are integers, if the
Poisson ratio of a matrix material is zero; thosederivatives of normalized stiffness elastic
constants forC33,C44,C11,andC66 converge to –1, –2, –3, and –4, respectively, at thecorresponding condition. We proposed a criterion of R<~1/3, where the mutual interaction
between pores becomes negligible for macroscopic composite elasticity.These derivatives arenearly constant below 5% porosity in the case of spherical pore, suggesting that the interaction
between neighboring pores is insignificant if the representative size of the pore is less than
one-third of the mean distance between neighboring pores. The relations we obtained in thiswork were successfully applied to invert bulk modulus and rigidity of Cmcm-CaIrO3 as a casestudy; the performance of the inverting scheme was confirmed through this assessment. Thus thepresent scheme is applicable to predict macroscopic elasticity of porous object as well.

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Semi Analytical Model for the Effective Grain Size Profile in the Mantle of the Earth
A. Rozel1, G. Golabek2, M. Thielmann2, P.J. Tackley1
1

ETH Zurich, 2Bayreurisches Geoinstitut
Corresponding author’s email address: antoinerozel@gmail.com
We present a semi analytical model of mantle convection able to predict the grain size
profile of the present day Earth. Grain size evolution has been studied with increasing interest
over the last decades but its behavior in both mantle and lithosphere remains largely
misunderstood due to its non-linearity. Several recent studies suggest that it might play afundamental role in localization of deformation in the lithosphere but we focus here on the
mantle in which we also observe important processes.
We propose a 1D compressible thermal convection model based on the equality of advective
heat flux and the integral of viscous dissipation in the whole domain. Imposing massconservation, our model is able to predict all rheological parameters able to produce both present
day average surface velocity and lower mantle viscosity. Composite rheologies involving
dislocation creep and grain size dependent diffusion creep are considered. The effect of phasetransitions on the grain size is also explicitely taken into account. We present the family ofsolutions for the activation volume and the viscosity jump at the 660 discontinuity according to
any initial choice of activation energy. The scaling laws for rheological parameters obtained arecompared to self-consistent evolutionary simulations of mantle convection considering grain size
dependent diffusion creep in 2D spherical annulus geometry.

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The Relationship of Crystallographic Orientation between Perovskite and Post-Perovskite
During Phase Transformation
D. Yamazaki1, M. Murakami2, F. Xu1, N. Hirao3, Y. Seto4
1

ISEI, Okayama University,
Graduate school of Science, Tohuku University
3
Japan Synchrotron Radiation Research Institute4
Kobe University
Corresponding author’s email address: dy@misasa.okayama-u.ac.jp
2

In the D” layer of the earth’s lower mantle is characterized by the seismic anomalies, forexample, velocity discontinuity, anisotropy and lateral heterogeneity [e.g., 1]. The dominant
phase in the D” layer is considered to be post-perovskite of (Mg,Fe)SiO3 and hence theirmineralogical properties are essential to understand the dynamics of the lower mantle. The
observed seismic anisotropy can be explained by the lattice preferred orientation of theconstituent materials [2]. One possible mechanism to form the lattice preferred orientation of
post-perovskite is topotactic relation between perovskite grain and post-perovskite grain duringphase transformation because the lattice preferred orientation of perovskite is likely formed due
to deformation during slab subduction. In this study, we investigated the topotactic relation bymeans of high pressure experiments in (Mg, Fe)SiO3 by using a diamond anvil cell and in CaIrO3
as an analogue by using piston cylinder apparatus.
In the series of experiments on CaIrO3, the coarse-grained polycrystalline perovskite was
firstly prepared as starting material. Then, at 1 GPa, the starting materials were partiallytransformed into perovskite. After experiments, the crystallographic orientation was determinedon the polished surface of the recovered sample by using electron back-scattered diffraction
technique. In the experiment on (Mg, Fe)SiO3, single crystal of perovskite was compressed to thestability field of post-perovskite (>120 GPa), and it was partially transformed to post-perovskite
as well as experiments on CaIrO3. In situ determination of crystallographic orientation was
performed by using synchrotron X-ray at SPring-8.
In the both series of experiments, we found the topotactic relation between the relict ofperovskite and the newly formed post-perovskite grain with a-axis of perovskite to b-axis of
post-perovskite, b-axis of perovskite to a-axis of post-perovskite and c-axis of perovskite toc-axis of post-perovskite (Fig. 1). The present results suggest that the lattice preferred orientationof post-perovskite is developed immediately after transformation from perovskite due to the
topotactic transition and then the pattern of lattice preferred orientation may be modified by thesubsequent deformation of post-perovskite in the D” layer.

Fig.1. Pole figure plots of CaIrO3 post-perovskite to perovskite.
References. [1] Panning and Romanowicz, (2004): Science, 303, 351; [2] Iitaka et al., (2004):Nature, 430, 442.
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Temperature of the Lower Mantle
C. Houser1, J. Hernlund1, R. Wentzcovitch2, J. Valencia-Cardona2
1

Earth-Life Science Institute, Tokyo Institute of Technology
2
University of Minnesota
Corresponding author’s email address: chouser@elsi.jp

The temperature is as much of an unknown as composition when considering the propertiesof the lower mantle. The temperature at the base of the mantle transition zone is constrained
within 100-200 K by interpreting depths of the 410 and 660 km seismic discontinuities as phasetransitions in a mantle with close to a pyrolite composition. The temperature at the core-mantle
boundary is constrained by observations of the post-perovskite phase transition and the melting
point of a pyrolite or perovskite composition. Pyrolite is the theoretical parent rock that canpartially melt to produce basaltic oceanic crust and a harzburgite oceanic lithosphere. Sinceoceanic lithosphere has been subducted and mixed in the Earth’s mantle for billions of years, it isreasonable to assume that the lower mantle could contain an abundance of material with close toa pyrolite composition. However, the Earth’s upper mantle appears depleted in Si relative tothe sun and most chondrite meteorites, so it may be that the lower mantle is more Si rich than theupper mantle. Since direct experimental measurements of rock velocity and density at actual
lower mantle temperatures and pressures are difficult, we currently rely on calculations ofvelocity and density to explore compositions/geotherms to test their compatibility withseismology and geodynamics. Since the community has not reached a consensus regarding
which technique is correct, here I present a variety of temperature profiles of the lower mantle
based on Density Function Theory as well as equation of state extrapolations using finite strain
theory. At low temperature, these methods are in generally good agreement, but differences
emerge above 2000 K, which constitutes most of the lower mantle. Since global seismic
observations can constrain the average seismic properties of the lower mantle, it has becomecommon practice to try to fit a computed velocity/density profile to a seismic model, such as
PREM, to examine whether or not a proposed composition could represent the dominant
mineralogy of the lower mantle. Results depend on the temperature profile which is often set
by defining the temperature at the top of the lower mantle and assuming the system is adiabatic
as pressure increases. The different methods agree that velocity and density increase as therelative amount of perovskite, or rather bridgmanite, increases, ie. Mg/Si ratio decreases. PREM
velocities are slower than pure perovskite and higher than ferropericlase, so some mixture of thetwo is needed to match the global seismic average. In the past, mixtures with a composition
close to pyrolite have been able to fit PREM with reasonable geotherms, but more Si enrichedcompositions required high temperatures to fit PREM. However, new calculations andexperiments suggest that the shear modulus may be lower than previously thought in the lower
mantle. In this case, the lower mantle could be more Si enriched or contain regions of Si
enrichment for more modest increases in temperature.

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Waveform Inversion for 3D Structure in D"
K. Kawai
Department of Earth Science and Astronomy
Graduate School of Arts and Sciences, University of Tokyo
Corresponding author’s email address: kenji@ea.c.u-tokyo.ac.jp
We formulate the inverse problem of waveform inversion for localized 3-D seismic structure,computing partial derivatives of waveforms with respect to the elastic moduli at arbitrary points
in space for anisotropic and anelastic media. In this study we minimize computational
requirements by using the Born approximation with respect to a laterally homogeneous model,
but this is not an inherent limitation of our approach. We solve the inverse problem using the
conjugate gradient (CG) method, using Akaike’s Information Criterion (AIC) to truncate the CG
expansion. We apply our method to invert for 3-D shear wave structure in the lowermost mantle
beneath Central America and the western Pacific at periods from 12.5 to 200 s for deep andintermediate-depth events. The resulting model beneath Central America shows lateralheterogeneity in the E–W direction, which may be associated with a subducted cold slab
surrounded by hotter materials with slower velocities [1]. We also find two low-velocity zones atthe bottom of the target region, with a high-velocity zone in the middle, and a low-velocity zone
above the high- velocity zone and contiguous with the two deeper low-velocity zones at a depthof 200–300 km above the core-mantle boundary (CMB) beneath the western Pacific. This
supports the idea that the Pacific LLSVP may be an aggregation of small upwelling plumes
rather than a single large thermochemical pile [2]. Various tests show that our model is robust.

References. [1] Kawai, K. et al. (2014): Geophys. J. Int., 197, 495–524; [2] Konishi, K. et al. (2014): Geophys. J.
Int., 199, 1245–1267

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Adjacent High- and Low-Velocity Regions around the Western Edge of the Pacific
Large-Low Shear Velocity Province
S. Tanaka
D-EARTH, JAMSTEC
Corresponding author’s email address: stan@jamstec.go.jp
The Large-Low Shear Velocity Provinces (LLSVPs) beneath Pacific and Africa are widely
recognized by global tomographic studies, which characterize the large-scale lateralheterogeneity in the lowermost mantle as well as high-velocity anomalies surrounding the
Pacific Ocean [1-3]. The detailed seismic wave analyses have suggested the existence of a sharpboundary of the LLSVPs [4, 5]. Especially, high velocity anomalies are fond to be adjacent tolow velocity anomalies near the western edge of the Pacific LLSVP for S-wave below New
Guinea [6] and P-wave below Micronesia [7]. Most recent study supports the similar S-wave
structure below Micronesia [8].
These results suggest that the material of subducted slabs is not easily assimilated into thesurrounding mantle, sometime deeply intruded in the LLSVP. This view is consistent with amantle dynamics simulation [9], which is based on a hypothesis that the dynamics of the
subducted slabs would affect the nature of the LLSVP and distribution of the ultra-low velocity
zones (ULVZ).
To confirm this hypothesis, further seismic data collection and analysis will be required. We
have a new project of a seismic observation, which aims to contribute to further understanding of
the structure and dynamics in such a complicated region.

References. [1] Ritsema, J. et al. (2010): Geophys J Int, 184, 1223-1236; [2] Lekic, V. et al. (2012): Earth Planet Sci
Lett, 357-358, 68-77; [3] French, S. and Romanowicz, B. (2015): Nature, 525, 95-99; [4] Rirsema, J. et al. (1998):
Geophys Res Let, 25, 4245-4248; [5] To, A. et al. (2005): Earth Planet Sci Lett, 233, 137-153; [6] Idehara, K., et al.
(2012): Geophys J Int, 192, 1-6; [7] Tanaka, S. et al. (2015): Geophys J Int, 200, 1052-1065; [8] Tanaka, S. and
Kawakatsu, H. (2015): JpGU 2015 meeting abstract; [9] McNamara, A. et al. (2010): Earth Planet Sci Lett, 299,
1-9.

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Technical Developments on Acoustic Emissions Monitoring at High Pressures
T. Ohuchi1, X. Lei2, Y. Higo3, Y. Tange3, T. Irifune1,4
1

Geodynamics Research Center, Ehime University
2
Institute of Geology and Geoinformation
National Institute of Advanced Industrial Science and Technology
3
Japan Synchrotron Radiation Institute4
Earth-Life Science Institute, Tokyo Institute of Technology
Corresponding author’s email address: ohuchi@sci.ehime-u.ac.jp
The subduction zone produces a major fraction of the Earth’s seismic activity.
Intermediate-depth earthquakes within the subducting slab form a double seismic zone. The
cause of intraslab seismicity have been attributed to dehydration of hydrous minerals. At deeper
depths, dehydration embrittlement (i.e., hydrofracturing) is expected to play an important role in
failure of rocks because the overall volume change of the dehydration reaction is positive andthus pore pressure can be increased [1]. However, experimental results on dehydration
embrittlement of antigorite are controversial. Dobson et al. [2] conducted a series of experiments
on dehydration of antigorite, and they reported that dehydration of antigorite associates acoustic
emission (AE) when the dehydration reaction is positive. Recently, Gasc et al. [3] reported thatno detectable AEs through dehydration of antigorite-rich serpentinite. Therefore, the cause ofintermediate-depth earthquakes is still unclear. In some of subduction zones, a significant
activity of deep-focus earthquakes has been reported [4]. It has been proposed that deep-focus
earthquakes are triggered by an instability faulting caused by olivine phase transformations [5].
Schubnel et al. [6] conducted deformation experiments on germanium olivine (Mg2GeO4) at 2-5
GPa and 1000-1250 K, and they observed many AEs generated in the sample. Schubnel et al. [6]discussed that fractures nucleated at the onset of the olivine-to-spinel transition.
To investigate the brittle properties of rocks, determination of AE source is critical. In thecommunity of high-pressure rock physics, Green & Burnley [7] conducted AE monitoring byusing a Griggs apparatus combined with an AE sensor. Dobson et al. [8] adopted 4 AE sensors toa multianvil apparatus. However, the position of AE source has not been determined in theexperiments because of not enough number of sensors used in the experiments. De Ronde et al.
[9] adopted 8 AE sensors to a multianvil apparatus and they succeeded to determine the positionof AE sources. Recently, Gasc et al. [3] succeeded to develop an experimental setup that allows
determining the position of AE source by using DIA-type multianvil apparatus combined with 6
AE sensors. Schubnel et al. [6] adopted the experimental setup reported by Gasc et al. [3]to a
D-DIA apparatus installed at a synchrotron facility, and they succeeded to measure strain andstress of the sample and AE signals. We have developed an experimental setup that is optimized
for the determination of the position of AE source in a synchrotron D-DIA apparatus. We willreport some preliminary experimental results on AE monitoring under the upper mantle
conditions.

References. [1] Raleigh, C.B. and Paterson M.S. (1965): J. Geoophys Res, 70, 3965-3985; [2] Dobson, D.P. et al.
(2002): Science, 298, 1407-1410; [3] Gasc, J. et al. (2011): Phys. Earth Planet. Inter, 189, 121-133; [4] Kirby, S.H.
et al. (1995): Geophys. Res. Lett, 22, 233-2236; [5] Kirby, S.H. et al. (1991): Science, 252, 216-225; [6] Schubnel, A.
et al. (2013): Science, 341, 1377-1380; [7] Green, H.W. and Burnley, P.C. (1992): Nature, 341, 733-737; [8]Dobson, D.P. et al. (2004): Phys. Earth Planet. Inter, 143-144, 337-346; [9] De Ronde, A.A. et al. (2007): Geophys.
J. Int, 171, 1282-1294.
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Creep Behavior of Fe-bearing Olivine under Hydrous Conditions
M. Tasaka1,2, M.E. Zimmerman 2, D.L. Kohlstedt2
1

Niigata University, 2University of Minnesota
Corresponding author’s email address: tasaka@geo.sc.niigata-u.ac.jp
Since iron and hydrogen plays an important role in dynamic processes not only in Earth's
mantle but also in Mars's mantle, we conducted uniaxial compression experiments on
polycrystalline samples of olivine, (Fe1-xFo, MgxFo)2SiO4, with XFo = 0, 0.53, 0.77, 0.90, and 1.0
under hydrous condition. A Paterson-type gas medium apparatus was used for these experiments.
The water content determined from Fourier transform infrared (FTIR) spectroscopy analyses oflarger Fo90 crystals embedded in the olivine polycrystalline aggregates demonstrate that the
samples are water saturated both before and after deformation. The grain sizes of initial anddeformed samples were determined using electron backscatter diffraction (EBSD).
Triaxial-compression tests at 300 MPa confining pressure were conducted at temperaturesfrom 1050 to 1200 °C at constant stress in the range of 25 to 316 MPa. The values of thepre-exponential term, stress and grain size exponents and activation energy in the constitutive
equation were determined for a wide range of XFo.
At constant temperature, strain rate, and grain size the flow stress of the samples decreases
with increasing iron content of olivine. Combining our data with that from Fe-bearing olivine
deformed under dry conditions (Zhao et al., 2009 EPSL), we formulated a flow law as a functionof XFo under both dry and wet conditions. The overall dependence of the strain rate of olivine on
XFo is characterized by 2 parameters, directly, through the exponent (m) in the coefficient X!
!" ofthe strain-rate and indirectly, through αXFo in the activation energy term, such as, (strainrate)=A*(stress)n/(grain size)p*(XFo)m*(water fugacity)r*exp[-(Q0+αXFo)/RT], where A is creep
constant, n is stress exponent, p is grain size exponent, m is iron content exponent, r is water
fugacity exponent, Q0 is activation energy coefficient, a is activation energy coefficient as afunction of XFo. Assuming an appropriate charge neutrality condition, the experimentally
determined value of m is well explained by the silicon vacancy concentration as a function of XFo.
Similarly, the dependence of the activation energy on αXFo can be correlated with a point defectmodel determined from thermo-gravimetric measurements for Fe-bearing olivine. These featuresindicate that if we know the charge neutrality condition and point defect model, we are able toreproduce the observed strain rate as a function of XFo, which may be applicable not only to theiron-bearing olivine but also to other solid solution systems.

References. [1] Tasaka, M., M. et al. (2015): J. Geophys. Res. Solid Earth, 120, doi:10.1002/2015JB012096.

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Stability Region of the (K, Na)AlSi3O8 Hollandite Solid Solution
Y. Zhou1, T. Irifune1,2, H. Ohfuji1, T. Shinmei1, W. Du1,2
1

2

Geodynamics Research Center, Ehime University, Matsuyama 790-8577, Japan
Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
Corresponding author’s email address: GRC2014917@gmail.com

Aluminosilicate hollandite, with a chemical formula of (K, Na)AlSi3O8, is a potential hostmineral of K in the deep mantle due to its stability [1] and abundance in high pressure phaseassemblages of K-rich compositions [2]. Phase relations in the system KAlSi3O8-NaAlSi3O8 are
important in understanding the behavior of the hollandite solid solution under high pressure andhigh temperature, but it remains unclear whether the Na hollandite end member is athermodynamically stable phase under some conditions or not. Previous studies reported that the
maximal solubility of NaAlSi3O8 in K hollandite was limited to 50 mol % [3,4], while most ofhollandite found in meteorites contain a large amount of Na, 80-90 mol % [e.g. 5,6]. Some DAC
experiments [7,8] identified trace NaAlSi3O8 hollandite in laser-heated albite compositions by
few fuzzy XRD peaks of hollandite, but the unsatisfactory XRD data and prevailing amounts ofcoexisting phases (CF NaAlSiO4 and stishovite) in the hollandite-containing product weaken the
conclusion about the stability of NaAlSi3O8 hollandite.
We investigated the phase relations in the system KAlSi3O8-NaAlSi3O8 at pressures of
20-23 GPa and temperatures of 1873 and 2273 K. The obtained phase relations are modally
consistent with those of the reference [3]: hollandite plus jadeite plus stishovite at relatively low
pressures, hollandite plus the calcium ferrite type NaAlSiO4 plus stishovite at relatively highpressures, and hollandite single phase when the Na content of the starting material is lower than
the solubility of NaAlSi3O8 in K hollandite at the corresponding condition. K hollandite
dissolves more NaAlSi3O8 component with pressure increase until the breakdown of jadeite atabout 22 GPa, and the Na content in K hollandite decreases substantially with further increasingpressure. The solubility of NaAlSi3O8 in K hollandite positively correlates with temperature, and
it is very sensitive to both pressure and temperature around the pressure corresponding to thedissociation of jadeite. Hollandite with Na content of 50 mol % was recovered at 22 GPa and1873 K, and Na-rich hollandite with 78 mol % Na was synthesized for the first time at 22 GPaand 2273 K. Lattice parameters of hollandite solid solutions decrease with increasing NaAlSi3O8
component. The improved phase relations can be used to estimate the composition of hollandite
in the Earth’s interior. The positive temperature dependence of the NaAlSi3O8 solubility in K
hollandite and the synthesis of Na-rich hollandite suggest a stability region for NaAlSi3O8
hollandite around 22 GPa at temperatures (slightly) higher than 2273 K, under which theformation of lingunite during meteorite impact can be elucidated via the phase equilibrium.

References. [1] Hirao, N.et al. (2008): Phys Earth Planet Inter, 166, 97-104; [2] Irifune, T. et al. (1994): Earth
Planet Sci Lett, 126, 351-368; [3] Yagi, A. et al. (1994): Phys Chem Miner, 21, 12-17; [4] Liu, X. (2006): Earth
Planet Sci Lett, 246, 317-325; [5] Gillet, P. et al (2000): Science, 287, 1633-1636; [6] Tomioka, N. et al. (2000):
Geophys Res Lett, 27, 3997-4000; [7] Liu, L. (1978): Earth Planet Sci Lett, 37, 438-444; [8] Tutti, F. (2007): Phys
Earth Planet Inter, 161, 143-149.

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Direct Sound Velocity Measurements of Pyrolite Across the Mantle Transition Region
S. Gréaux1,2, T. Irifune1,2, M. Nishi1, Y. Higo3, T. Inoue1, T. Arimoto1, Z. Liu1
1

Geodynamics Research Center, Ehime University,
Earth-Life Science Institute, Tokyo Institute of Technology,
3
SPring-8, JAMSTEC
Corresponding author’s email address: greaux@sci.ehime-u.ac.jp
2Comparison of seismic data with laboratory sound wave velocities in minerals at
high-pressure and high temperature plays a major role in interpreting the variations incomposition as a function of depth in the Earth’s interior. Although numerous studies haveinvestigated the sound velocities of minerals under high pressure and high temperature (see a
review by Li and Liebermann [1]), it is still debated that the pyrolite model explains well theseismic velocity profiles of seismological reference models. To this day, mantle velocities are
estimated by averaging data from single phase studies [2], sometime using results from thoseusing different techniques. In addition, only few of those experiments were conducted at pressure
and temperatures relevant to the Earth’s deep interior.
Here we investigated directly the velocities of pyrolite aggregates at pressures up to 30 GPa
and temperatures up to 1700 K, which correspond to the lowermost part of the Earth’s lower
mantle. High pressure and high temperature sound velocities of pyrolite were measured by theultrasonic interferometry method combined with synchrotron radiation techniques in a large
volume press. Starting materials consisted of polycrystalline aggregates with a pyrolite bulk
composition. Samples hot-pressed at 10 GPa consisted of Olivine (Ol), Garnet (Gt) andPyroxenes (Px) while those synthesized at 17 GPa and 27 GPa respectively consisted of
Wadsleyite (Wd) and Majorite garnet (Mj); and Bridgmanite (Br), Periclase (Pc) and CaSiO3
perovskite (CPv).
We observed a clear contrast in between the velocities of the Ol+Gt+Px assemblage
compared to those of Wd+Mj in agreement with the Olivine-to-Wadseleyite transformation at~14 GPa [3]. The velocity gradients associated with phase transformations are well consistent
with PREM [4] in the lowermost transition region but fail to explain its uppermost part
especially at the 410 km depth discontinuity. Velocities at pressures higher than 25 GPa are alsopresented and the overall data discussed relative to the mineralogical composition of the mantle
across the transition region.

References. [1] Li, B. and Liebermann, R.C. (2014): Phys. Earth Planet. Int, 233, 135-153; [2] Irifune, T. et al.
(2008): Nature, 451, 814-817; [3] Katsura, T. et al. (2004): J. Geophys. Res. B, 109. [4] Dziewonski, A.M. andAnderson, D.L. (1981): Phys. Earth Planet. Int, 25, 297-356.

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Effects of the Subducted Slab on Dynamics of the Lowermost Mantle
T. Kaneko, T. Nakakuki
Department of the Earth and Planetary Systems Science, Hiroshima University, Japan
Corresponding author’s email address: d154713@hiroshima-u.ac.jp
The structure and evolution of the Earth’s lowermost mantle must be significantly
influenced from subduced slabs, as seismological studies indicate that the slabs penetrate into thelower mantle. Seismological studies also suggest prominent features on the morphology (e.g.
high elevation, steep edge [1], correlation between margin and hot spot locations [2]) and thestability (e.g. existence over a long term [2]) of the large low shear velocity provinces (LLSVPs)
that exist at the base of the mantle. We perform a numerical study to investigate that influence ofthe lower mantle properties on the mechanical interactions of the subducted slab with apost-perovskite phase change and a compositionally dense layer by using a 2-D Cartesian model.
Our model simulates a whole mantle convection system in which plate-like motion isrealized without any forces imposed on the lithosphere. Therefore we can observe the evolutionof the lowermost mantle structure coupled with natural subducted slab behavior. We introduce achemically distinct segment with the density increase of 77.3 kg m-3 and the post-perovskite
phase change with the Clapeyron slope of +8 MPa K-1 and the density contrast of 49.9 kg m-3.
We also incorporate phase diagrams of hydrous minerals [3] and hydration effects on the density
and the viscosity [4]. In this study, we focus on the following parameters that affect the slab
subducting history and the evolution of the dense layer; depth profile of the background mantle
viscosity, depth dependence of a thermal expansivity and yield strength of the slab.
The viscosity profiles effects on not only the slab sinking velocity, but also temperature anddeformation of the dense layer. The small viscosity of the lower mantle results in temperature
increase in the whole potion of the chemically dense segment due to effective convection in theinside of the segment. Therefore, a thermal boundary layer is developed above the chemicallydense segment. Moreover, the dense layer tends to significantlly deform by strong mantle flow
induced by the rapid subducted slab motion. When the lower mantle viscosity is as higher as 1022
Pa s, the thermal boundary layer over the CMB, however, grows up without the development ofsmall-scale convection in the dense layer. The slab yield strength has effects on the subducting
slab structure when the thermal expansivity is constant. In the cases with the yield strength of
200 MPa, the subducting slab experiences buckling. The thermal expansivity plays importantroles in the stability of the dense layer and a system of rising plumes. When the thermal
expansivity is constant, the dense segments deform strongly and rise off the CMB by the
subducted slab plunging into the dense segment. On the other side, a thermal expansivity
decreasing with depth stabilizes the dense structure. Furthermore, the upwelling plumes are
generated on the top of the dense structure.

References. [1] Ni, S. et al. (2002): Sience, 296, 1850-1852; [2] Torsvik, T. H. et al. (2006): Geophys. J. Int, 167,
1447-1460; [3] H. Iwamori. (2004): Earth and Planetary Science Letters, 227, 57-71; [4] S. Karato. and H. Jung
(2003): Philosophical Magazine, 83, 401-414.

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Single Crystal Elasticity of the Lower Mantle Minerals Using Inelastic X-ray Scattering
H. Fukui1,2, A. Yoneda3, A.Q.R. Baron2
1

Graduate School of Material Science, University of Hyogo
Materials Dynamics Laboratory, RIKEN SPring-8 Center
3
Institute for Study of the Earth’s Interior, Okayama Univeristy
Corresponding author’s email address: fukuih@sci.u-hyogo.ac.jp
2

Experimental study on single crystal elasticity of the earth’s lower mantle materials is
important to understand chemical and thermal structures of the earth’s interior. Some synthesized
samples of the lower mantle materials are tiny and opaque. Inelastic X-ray scattering technique isa powerful tool to investigate that property of these samples [1].
We have performed IXS measurements on CaIrO3 with a Cmcm postperovskite structure [2]and (Mg,Fe,Al)(Si,Al)O3 with a Pbnm perovskite structure [3] and revealed their full elastic
stiffness matrices. The Cmcm-CaIrO3 is an analogue material of Cmcm-MgSiO3, which isconsidered a main component of D″ layer just above the Earth’s core–mantle boundary. The
diversity of elastic wave velocity in D″ layer [4] can be explained from latticepreferredorientation and seismic anisotropy of the analogue material. We have experimentally found thatcation substitution makes the single crystal elasticity of Pbnm-(Mg,Fe,Al)(Si,Al)O3 moreanisotropic and, makes bulk and shear moduli larger and smaller, respectively (Figure 1). Thiscan explain the seismic anti-correlated anomaly observed in the deep lower mantle [5].

Figure 1. Stereo projections of elastic wave velocities of Pbnm-(Mg,Fe,Al)(Si,Al)O3, bridgmanite based on elastic
stiffness constants determined by inelastic x-ray scattering. The crystallographic directions a, b, and c are shown inpanel (a). The unit of scale bars in m·s−1. (a-c) VP, average of two VS, and difference between two VS, respectively,
for MgSiO3 bridgmanite. (d-f) Those for Fe and Al bearing one.

References. [1] Fukui, H. et al. (2008): Journal of Synchrotron Radiation, 15, 618-623; [2] Yoneda, A.et al. (2014):
Nature Communications, 5, 3453; [3] Fukui, H. et al.(submitted); [4] Lay, T. and Garnero, E. (2011): Annual Review
of Earth Planetary Science, 39, 91-123; [5] Trampert J. et al. (2004): Science, 306, 853–856.

40	
  
	
  

	
  

Thermal Equation of State of MgSiO3 Post-perovskite
T. Sakai1, H. Dekura1, N. Hirao2
1

Geodynamics Research Center, Ehime University
2
Japan Synchrotron Radiation Research Institute
Corresponding author’s email address: sakai@sci.ehime-u.ac.jp
We established thermal equations of state (EoS) of MgSiO3 post-perovskite phasedetermined both by laser-heated diamond anvil cell (LHDAC) and density-functional theoreticaltechniques. The LHDAC experiments were performed up to a pressure (P) of 265 GPa attemperature (T) of 300 K and 170 GPa at 2560 K. The ab initio calculations were performed up
to 1.2 TPa and 6000 K. The Keane and AP2 equations of state models at multi-megabar rangethat include parameters at high-pressure limit to infinity were adopted for the first time to extract
some meaningful physical properties. The volume data experimentally obtained in the wide
pressure-temperature range were then applied to the Mie-Grüneisen-Debye model with fully
experimental parameters. The Grüneisen parameter and its volume dependency were foundconsistent perfectly with the theoretically obtained ones. Both the experimental and theoretical
EoSs are also found in very good agreement with each other within 0.1% in volume at the earth’s
core-mantle boundary condition, and the relation keeps within 0.8% even up to 300 GPa and6000 K. Our newly developed EoSs should be applicable to the super-Earth’s mantle as well as
the Earth’s core-mantle boundary region.

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Experimental Identification of a New Pyrite-type Hydroxide at Multimegabar Pressures
M. Nishi1,2, Y. Kuwayama1,2, J. Tsuchiya1,21

Geodynamics Research Center, Ehime University
Earth-Life Science Institute, Tokyo Institute of Technology
Corresponding author’s email address: nishi@sci.ehime-u.ac.jp
2

The discovery of the new high pressure hydrous minerals has the important implications forthe structure, dynamics and evolution of the Earth, since the hydrogen in the mantle hassignificant effects on the physical properties and stabilities of constituent minerals in the Earth.
In order to understand the global circulation mechanism of hydrogen in the Earth, a number ofhigh pressure experiments on hydrous phases have been conducted. The recent discovery of newhydrous minerals, phase H and δ-AlOOH with very similar crystal structures, implies that the
deep water subduction can reach to the bottom of the lower mantle. However, studies on thestabilities of hydrous minerals at pressures higher than those of the Earth’s mantle have been
scarce, in spite of their importance for exploring the potential presence and role of water ingigantic planets. In-situ X-ray diffraction experiments on AlOOH were performed using alaser-heated diamond-anvil cell (DAC) technique to investigate the stability and phase transitionof hydroxide at high pressures. We succeeded to observe the phase transition of δ-AlOOH to apyrite-type structureat above 190 GPa and 2500 K with an increase in density of 2.6 %. The
result is supported by first-principles density-functional calculations, which predict the
pyrite-type AlOOH stabilizes at above 170 GPa. The stability of the pyrite-type hydroxide at theextreme high pressure may affect the modeling on the internal structure and deep water circle ofsome extra-solar planets.

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Technical Developments in High Temperature Generation with Sintered Diamond Anvils
T. Arimoto1, T. Irifune1,2, M. Nishi1,2, Y. Tange3, T. Kunimoto1
1

2

Geodynamics Research Center, Ehime University,
Earth-Life Science Institute, Tokyo Insitute of Technology, 3JASRI
Corresponding author’s email address: arimoto@sci.ehime-u.ac.jp

Kawai-type multi-anvil apparatus (KMA) with sintered diamond (SD) anvils is a powerfulapparatus to provide high pressure and high temperature condition corresponding to Earth’s
lower mantle. To date, a number of studies on the high pressure generation using SD anvils havebeen reported [e.g. 1, 2], and Yamazaki et al. (2014) achieved pressures up to 109 GPa. However,
the high temperature generation corresponding to mantle geotherm over 50 GPa region has beenquite difficult. In this study, we report recent works for technical developments in hightemperature generation using SD anvils.
High pressure and high temperature experiments were carried out at BL04B1 beamline,
SPring-8, and geodynamics research center, Ehime University. Two KMA (SPEED-Mk.II and
MADONNA II) were used. SD anvils with TEL 1.5 mm were used. Pressure was calculated by
the equation of state of gold [3], and temperature was monitored by a W97Re3-W75Re25
thermocouple placed adjacent to a sample. A LaCrO3 and a cylindrical Re were used as a heater.
We optimized the cell assembly for SD anvils in order to improve efficiency of pressure andtemperature generations, and achieved the maximal pressure to 64 GPa at 6.0 MN. Hightemperature generation to 2000 K was made at 59 GPa. Performance of LaCrO3 heater was quite
stable without any scattering at that pressure region during 2 hours. On the other hand, the higher
temperature generation (2773 K) using Re heater was reported by Ito et al. (2004) [4]. Therefore,
we additionally tested the Re heater combined with assembly for SD anvils.

References. [1] D.Yamazaki et al. (2014): Phys Earth Planet. Inter, 228, 262-267; [2] Y.Tange et al. (2008): HighPres. Res, 28, 245-254; [3] T. Tsuchiya. (2003): J. Geophys. Res, 108, B10, 2462; [4] E. Ito et al. (2004): Phys
Earth Planet. Inter, 143-144, 397-406.

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Over 3000°C Generation in Kawai-Cell Byboron-Doped Diamond Cylinder Heater
L.J. Xie, Akira Yoneda, Eiji Ito
Institute for Study of the Earth’s Interior, Okayama University
Corresponding author’s email address: p1f77h4y@s.okayama-u.ac.jp
It is the first report of synthesizingsemi-conductor boron-doped diamond (BDD) cylindricalheaterin the Kawai-type multi-anvil apparatusat 15 GPa and 2100°C. The dimension of thecylindrical heaters was2.6/1.5/3.35 mm in order of outer diameter, inner diameter, andlength.SEM image shows that the grain size of diamond is about 1 µm.
Thecylindrical heaterwastestedfor extremely high temperature generation in a large sample
volume (~0.1mm3) in the Kawai apparatus; the sample volume is ~1000 times larger than that indiamond anvil cell.Thisworkwasthe first trialofpre-synthesizedBDD heater in Kawai-typeapparatus.The reproducibility of the BDD heater was confirmed well through three times ofrepeated cycles of heating and cooling.The BDD heater with 3 wt.% boron showedmetallic
behavior, i.e. increasing resistance with increasing temperature. This electricalcharacteristicwasbeneficial forstablegeneration oftemperature as high asup to 2700°C; theheating for further higher temperature was failedowing to thedeteriorationof electrode.
We succeeded to generate temperature up to ~3500 °C by using a smaller BDDheater(1.5/1.0/6.0 mm) and TiC electrode. We molded this heater from BDD powder to overcome thedifficulty synthesizing such a thin BDD cylinder at high pressure.Temperatures higher than1800 °C were estimated from the input power based on its power-temperature relationshipbefore
the break ofthermocouple. The effect of the hard BDD heater onpressure
generationwasexaminedin thein-situ X ray experiment at SPring-8.
BDD heateris free from complicated power-temperature relationship and pressure drop
associatedwith graphite-diamond conversion. Thus it is much more advantageous than boron
doped graphite heater.

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Properties of Liquid Iron Alloys under Extreme Conditions
G. Morard1, D. Andrault2, D. Antonangeli1, J. Siebert1, F. Guyot1, A.L. Auzende1, O. Lord3,
J.Bouchet4, M.Harmand1, B.Cochain5, G.Garbarino6, I.Kantor6,
R.Torchio6, E.Boulard6, M.Mezouar6
1

IMPMC. CNRS. Université Pierre et Marie-Curie, Paris, France
2
Laboratoire Magmas et Volcans, Clermont-Ferrand, France
3
School of Earth Sciences, University of Bristol, Wills Memorial Building,Queen’s Road, Bristol, BS8 1RJ, UK
4
CEA, DAM, 91297 Arpajon, France
5
Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy
Centre for Science at Extreme Conditions (CSEC)
University of Edinburgh, Edinburgh, EH9 3JZ, UK
6
European Synchrotron Radiation Facility, Grenoble, France
Corresponding author’s email address: guillaume.morard@impmc.jussieu.fr
The major portion of the Earth’s core is in the liquid state, accounting for 18% of the total
planetary volume. Although mostly composed of iron, it contains impurities that lower its
density and melting point with respect to pure Fe. It is therefore important to determine melting
relations and melting temperature of iron alloys under extreme conditions to constrain thermal
structure and dynamic of the Earth’s core. Although, with the recent discovery of extra-solar
planets, planets with similar structures and masses up to 10 times the mass of the Earth open newquestions concerning properties of iron and iron alloys under extreme conditions (330-1500 GPa,
5000-10000K), with potentially a large portion that is in the liquid state. Here we will present
way to investigate iron and its alloys from conditions of Earth’s to Super-Earth’s cores.
We will present XRD and XANES experimental results on liquid iron alloys measured using
the Laser-Heated Diamond Anvil Cell (LH-DAC) up to multi-megabar conditions, obtained
respectively on ESRF beamlines ID27 and ID24. We will discuss how each light element affectthe local structure and the phase diagram of pure iron.

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Liquid Iron Alloys with Hydrogen at Outer Core Conditions by First Principles
K. Umemoto1, K. Hirose1,2
1

Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo, Japan
2
Laboratory of Ocean-Earth Life Evolution Research
Japan Agency for Marine-Earth Science and Technology, Kanagawa, Japan
Corresponding author’s email address: umemoto@elsi.jp
Since the density of the outer core deduced from seismic data is about 10% lower than that ofpure iron at core pressures and temperatures (P-T), it is widely believed that the outer coreincludes one or more light elements. Although intensive experimental and theoretical studies
have been performed so far, the light element in the core has not yet been identified. Comparisonof the density and sound velocity of liquid iron alloys with observations, such as the PREM, is apromising way to determine the species and quantity of light alloying component(s) in the outercore. Here we report the results of a first-principles molecular dynamics study on liquid ironalloyed with hydrogen, one of candidates of the light elements. Hydrogen had been much lessstudied than other candidates. However, hydrogen has been known to reduce the melting
temperature of Fe-H solid [1]. Furthermore, very recently, Nomura et al. argued that the outer
core may include 24 at.% H in order to be molten under relatively low temperature (< 3600 K)[2]. Since then hydrogen has attracted strong interests. We clarify the effects of hydrogen on
density and sound velocity of liquid iron alloys under outer core P-T conditions. It is shown that
~1 wt% hydrogen can reproduce PREM density and sound velocity simultaneously very well. In
addition, we show the presence of hydrogen rather reduces Grüneisen parameters. It indicates
that, if hydrogen exists in the outer core, temperature profile of the outer core could be changed
considerably from one estimated so far.

References. [1] Sakamaki, K. et al. (2009): Phys. Earth Planet. Inter, 174, 192-201; [2] Nomura, R. et al. (2014):
Science, 31, 522-525.

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Core Liquids: Fact and Fiction
G. Helffrich
Earth-Life Science Institute, Tokyo Institute of Technology
Corresponding author’s email address: george@elsi.jp
The heat flowing through the core-mantle boundary is a control on the conditions forconvection in the mantle [1] and for the cooling of the core from its initial stateand developmentof its dynamo [2]. Recent work on measuring core metal transport properties at high pressuresand temperatures [2] shows that the core transfers heat more readily than the best-guess
extrapolations from ambient conditions, and poses problems for the long-term viability of thegeodynamo as it operates today. One remedy is that long-term core stratification reduces the heattransfer rate due to thermal or chemical stratification. This prolongs the growth of the inner coreallowing a dynamo by release of chemical buoyancy at the inner core boundary.
There is evidence that parts of the outer core are not in a well-mixed, adiabatic state,particularly the top of the core where heat transfer to the mantle takes place [3]. Some view thisevidence as controversial because it does not correspond to their belief that adding any lightelement to iron liquid necessarily raises seismic wavespeeds [4]. This belief is buttressed by firstprinciples calculations of liquid iron alloy wavespeeds that uniformly show rising seismic
wavespeeds with rising light element concentration [5]. However, experimental data foriron-sulfur mixtures unequivocally show that seismic wavespeeds decrease as more sulfur isadded. Hence the prevailing belief needs revision in the face of actual data. To advanceunderstanding of the core's properties and of Earth evolution, we need to pursue a market basket
of approaches that are anchored to observational data rather than beliefs. I outline one approachinterpreting the seismic wavespeed variations in the top of the outer core.

References. [1] Labrosse, S. et al. (2007): Nature, 450, 866-869; [2] Gomi, H. et al. (2013): Phys. Earth and Planet.
Int, 224, 88-103; [3] Helffrich, G. & Kaneshima, S. (2010): Nature, 468, 807-810; [4] Buffett, B. & Seagle, C.
(2010): J. Geophys. Res, 115; [5] Badro, J. et al. (2013): Proc. Nat. Acad. Sci, 111, 7542-7545.

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Crystallization of SiO2 in Earth's Core after High-temperature Core Formation
K. Hirose1, G. Morard2, H. Ozawa3,
G. Helffrich1, J. Hernlund1
1

2

Earth-Life Science Institute, Tokyo Institute of Technology
IMPMC, Universite Pierre-et-Marie-Curie, 3Okayama University

Recent core formation models based on the metal–silicate partitioning of siderophileelements suggest that the Earth's core was formed by metal segregation from silicate at highpressure and high temperature in a deep magma ocean. It is also known that the simultaneous
solubility of silicon and oxygen in liquid iron are strongly enhanced at high pressure and hightemperature, such that at the end of accretion the core was rich in both silicon and oxygen.Here
we performed crystallization experiments on the Fe–Si binary and Fe–Si–O ternary systems up
to core pressure in a laser-heated diamond-anvil cell. Thestarting material for the latter was ahomogeneous mixture of fine-grain Fe-Si and SiO2 (<1µm). We prepared cross sections ofsamples recovered from the DAC usinga focused ion beam (FIB) and subsequently performed
textural and chemical characterizationwith field-emission-type electron microprobe (FE-EPMA).
Quenched liquid alloy was found at the hottest part coexisting with a solid phase (liquidus phase)at theperiphery. These results combined with literature data on the melting phase relations in the
Fe–FeO binary system demonstrate that the liquidus field of SiO2 is very wide at the Fe-rich
portion of the Fe–Si–O ternary system at the core pressure range. It indicates that the original
Fe–Si–O core liquid should have crystallized a large amount of SiO2 until it lost either silicon or
oxygen. The recent finding of high thermal conductivity of the core suggests that core thermal
convection is difficult to sustain without extreme degrees ofsecular cooling.However,even formodest degrees of joint Si-O incorporation into the early core, the buoyancy released by
crystallization of SiO2issufficient to overcome thermal stratificationand sustain the geodynamo.

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Linking Seismic Observations of Earth's Inner Core
Boundary to Deeper Structure
L. Waszek1, A. Deuss2, H. Godwin3
1

University of Maryland College Park, 2University of Utrecht, 3University of Oxford
Corresponding author’s email address: lauren.waszek@cantab.net

The inner core boundary marks the phase transition between the solid inner core and thefluid outer core. As the site of inner core solidification, the boundary provides insight into
theprocesses generating the seismic structures of the inner core. In particular, it may hold the key
tounderstanding the previously observed hemispherical asymmetry in inner core seismic
velocity,anisotropy and attenuation. Here, we use a large PKiKP-PcP amplitude ratio and travel
timeresidual dataset to investigate velocity and density contrast properties near the innercoreboundary. Although hemispherical structure at the boundary has been proposed bypreviousinnercore studies, we find no evidence for hemispheres in the amplitude ratios or travel
time residuals.
The amplitude ratios are much larger than predicted, and show no regional coherency, while
thetravel time residuals display large regional variations.Beneath the inner core boundary,previous studies have constrained the hemispherical seismicvelocity structure in the Earth's innercore at depths greater than 15 km below the inner coreboundary. However, the properties ofshallower structure have not yet been determined, becausethe seismic waves used for analysis
arrive close together and interfere. The uppermost layer ofthe inner core was formed mostrecently, thus is most strongly correlated to the inner coresolidification processes and structuresat the inner core boundary.To study this upper region, wepresent a new waveform modelingmethod to measure the seismic velocity in the top 15 km ofthe inner core. As proof of concept,
we apply our method to an event with ray paths which traverse the Pacific hemisphere boundary.
Our preliminary observations indicate hemisphericalstructure in the uppermost layers of theinner core, despite no hemispherical structure at the boundary itself.

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Freezing and Melting above the Inner Core Boundary
M. Lasbleis1, J. Hernlund1, S. Labrosse2
1

Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo
2
Laboratoire de Géologie de Lyon, ENS de Lyon, France
Corresponding author’s email address: marine.lasbleis@elsi.jp

Seismic observations of the Earth’s core reveal a complex structure: radial and lateralheterogeneities in seismic anisotropy and attenuation in the solid inner core, but also
discrepancies between observed P-wave velocity and homogeneous PREM model in the deep
liquid outer core. [1] showed that no published large-scale dynamical model can explain thewhole complexity of the inner core, as seen by the seismic observations. Here we want to focus
on the freezing and melting processes that occur at the inner core boundary and above.
In particular, the 200km anomalous layer at the bottom of the outer core exhibits seismic
velocities lower than the PREM model. It has been interpreted as a layer depleted in lightelements, whereas the usual model considers that light elements are expelled at the surface of theinner core by freezing of the outer core alloy. Recent models of core formation argued for an
early stratified liquid core, and the stratified layers at the top and bottom of the outer core would
be a vestige of this primordial stratification. However, freezing of the inner core at the inner coreboundary releases light elements that provide buoyancy fluxes that would mix the stratified
liquid above with small-scale buoyant plumes. To model the F-layer, we consider that thefreezing of the iron alloy and the release of light elements have to occur in the bulk of the layer.
Iron snow forms and settles in the layer, buffering the thermal and chemical profile to theliquidus. We show that this dynamics can both sustain and stabilise the stratified layer in theliquid outer core while simultaneously matching the seismic observations.

References. [1] Lasbleis, M., & Deguen, R. (2015): Physics of the Earth and Planetary Interiors.

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Thermal Structure of the Inner Core Boundary in Numerical Dynamos
H. Matsui
Department of Earth and Planetary Sciences, University of California, Davis
Corresponding author’s email address: hrmatsui@ucdavis.edu
Seismic anisotropy through alignment of crystal lattices suggests aspherical growth of theinner core. Slow viscous deformation of the inner core and latent heat distribution by flow
motion are expected to be the origin of the aspherical growth of the inner core. In Buffett andMatsui (2015)[1], the temperature heterogeneity at ICB was prescribed and investigated a changeof largescale flow due to this heterogeneity. In the present study, we solve
magnetohydrodynamics (MHD) simulation in a rotating spherical shell with considering the heat
equation in the inner core. To compare the results with the simulation without considering theinner core, we assume that the inner core is electrically insulated and co-rotate with mantle. In
addition, we set the same thermal diffusivity for the inner core and outer core, and introduce a
constant heat source in the inner core to keep the average temperature in the outer core throughthe simulations. We also set a homogeneous heat flux at the outer boundary of the shell as athermal boundary condition at CMB. We compare the simulations results with the simulations
results using fixed heat flux or temperature condition at ICB.
The results show that larger temperature heterogeneity is generated than the heat flux at ICB
because heat flux at ICB has smaller length and time scale comparing with the temperature
variation at ICB. In these results, a large temperature variation is observed at the both ICB and
CMB. The range of the variation is approximately 0.9 times of the average temperature
difference between ICB and CMB. The largest temperature variation is observed in Y20
component in the spherical harmonics. i.e., higher and lower temperature is observed at the poles
and equator, respectively. This temperature pattern at ICB also reflects the temperature pattern at
CMB. We observe the high temperature patch at the pole, while lowest temperature is observedin the fixed temperature ICB case. On the other hand, Y11 component, which can generate atransition mode in the inner core, is approximately 0.1 times of the Y11 component and drifts inthe zonal direction for approximately a half of the magnetic diffusion time. Consequently, Y20
component remains as a stable temperature heterogeneity at ICB.
We do not take into account for the latent heat in the present simulations. Constructing amodel including the latent heat at ICB will be the next study. We expect that the latent heat willstabilize the temperature heterogeneity at ICB in the present study. However, present results will
be good reference to compare the model with the latent heat.

References. [1] Buffett, B.A, and Matsui, H. (2015): Physics of the Earth and Planetary Interiors, 243, 22-29.

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Lattice Preferred Orientation of Hcp-Iron Induced by Shear Deformation
Y. Nishihara1, T. Ohuchi1, T. Kawazoe1,2, G. Maruyama1,
Y. Higo3, K. Funakoshi3,4, Y. Seto5
1

Geodynamics Research Center, Ehime University, 2BGI, Bayreuth University
3
JASRI, 4CROSS-Tokai, 5Kobe University
Corresponding author’s email address: yunishi@ehime-u.ac.jp

Many hypotheses have been proposed for origin of seismic anisotropy in the Earth’s innercore which consists of solid metal. Plastic deformation of constituent material (most probably
hexagonal-close-packed (hcp) iron) is one of the candidate processes to form the inner coreanisotropy (e.g. [1]). Thus knowledge of deformation-induced lattice preferred orientation (LPO)of hcp-iron is important for understanding of nature of the inner core. Only limited numbers ofexperimental studies have been reported on deformation induced LPO of hcp-iron because thisphase is unquenchable to ambient condition. In the previous studies, hcp-iron was deformed byuniaxial compression, and slip activities in deforming sample were indirectly estimated based onelastoplastic self-consistent modeling (e.g. [2]). In this study, we have carried out shear
deformation experiments on hcp-iron and determined its deformation induced LPO.
Shear deformation experiments of hcp-iron were carried out at pressure of 9–18 GPa andtemperature of 723 K using a D-DIA apparatus, SPEED-Mk.II-D, installed at BL04B1, SPring-8[3]. In the deformation experiments, pressure medium of 4.5 or 5.0 mm (Mg,Co)O cube and WC
and cBN second stage anvils with 2.5 or 3.0 mm truncation were used. The sample iron was
sandwitched between two 45º-cut Al2O3 pistons in the cell assembly. Shear strain rates in theexperiments were ~2 × 10–4 or ~0.6 × 10–4 s–1, and total shear strain is ~2. Development of LPO
in the deforming sample was observed in-situ based on two-dimensional X-ray diffraction using
an imaging plate detector and monochromatized synchrotron X-ray with energy of 49–51 keV.
LPO of sample was determined from the two-dimensional diffraction pattern using a software
ReciPro 2 [4].
_In shear deformation of hcp-iron, <0001> and <112 0> axes gradually aligned to be
sub-parallel to shear plane normal and shear direction, respectively, from initial random_orientation. The <0001> and <1120> axes are back-rotated from shear direction by ~30º. The_

above results suggest basal slip <1120>{0001} is the dominant slip system under the studied
deformation conditions. It has been shown that Earth’s inner core has an axisymmetricanisotropy with P-wave traveling ~3% faster along polar paths than along equatorial directions.
Although elastic anisotropy of hcp-iron at the inner core conditions is still controversial, recent
theoretical studies consistently shows that P-wave velocity of hcp-iron is fastest along <0001>
direction at least at low-temperatures. Our experimental results could be suggesting that mostpart of the inner core deforms with shear plane sub-parallel to equatorial plane (e.g. [5]).

References. [1] Sumita, I & Bergman, M.I. (2009): Treatise on Geophysics8, Core Dynamics, 299-318; [2] Merkel,
S., et al. (2004): Phys. Earth Planet. Int, 145, 239-251; [3] Kawazoe, T. et al. (2011): Am. Mineral, 96, 1665-1672;[4] Seto, Y. (2012): Rev. High Press. Sci. Tech, 22, 144-152; [5] Wenk, H.-R. et al. (2000): J. Geophys. Res, 105,5663-5677.

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View and Perspectives on the Lower Mantle from Geo-neutrinos
S.T. Dye1,21Department of Physics and Astronomy, University of Hawaii, Honolulu, HI 96822, USA
2
Department of Natural Sciences, Hawaii Pacific University, Honolulu, HI 96814, USA
Corresponding author’s email address: sdye@phys.hawaii.edu

We explore the capacity for geo-neutrino observations to estimate the quantity anddistribution of radiogenic elements in the lower mantle. Geo-neutrinos originate as electron
antineutrinos from the beta-minus decays of 40K and of daughter nuclei in the decay series of232
Th, 238U, and 235U. The long lifetimes of these isotopes make potassium, thorium, and uranium
the main radiogenic, heat-producing elements in Earth. Neutrino emission from beta decay isisotropic, and neutrinos of all types carry no electric charge, allowing direct passage throughelectric and magnetic fields. Neutrino particle states have different masses, producing harmonic
fluctuations of neutrino interaction states along the direction of travel. Because the wavelengthof geo-neutrino oscillations is short compared with the size of geological reservoirs, anapproximately constant reduction in the surface flux applies. The direction and energy spectrumof the geo-neutrino flux at the surface provide a unique, model-independent image of radiogenic
reservoirs within Earth. Sufficient exposure of detectors, sampling over the surface of Earth,provides neutrino emission tomography of the planet. Geo-neutrino interactions with mater are
extremely rare, requiring well-shielded, massive, and long-term detector projects in deep
underground, and potentially underwater, locations.
Two inaugural underground detectors, one in Japan and one in Italy, are sampling the energy
spectrum but not the direction of the geo-neutrino flux. In addition to geo-neutrinos, thesedetectors measure antineutrinos from nuclear reactors. Reactor antineutrinos are a dominantsource of background to the geo-neutrino signal. The reported observations from the two
detectors are consistent with one another, providing no model-independent evidence for the
existence of geological reservoirs with different concentrations of radiogenic elements.
Estimating the quantity and distribution of radiogenic elements in the lower mantle bygeo-neutrino measurements is a formidable task. It is probably most directly realized by
geo-neutrino observations in the deep ocean and by developing the capability to measure thedirection of the geo-neutrino flux. We discuss these possible achievements, describe recent
progress on modeling the reactor antineutrino background, and present observational strategies
for gaining perspective on the lower mantle.

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Geo-neutrino Measurement with KamLAND and Future Prospects
H. Watanabe
Research Center for Neutrino Science, Tohoku University, 6-3
Sendai, Miyagi, 980-8578, JAPAN
Corresponding author’s email address: hiroko@awa.tohoku.ac.jp
The KamiokaLiquid-scintillator Anti-Neutrino Detector (KamLAND) is located in a rockcavern in the Kamioka mine, 1,000 m below the summit of Mt. Ikenoyama in Japan.
KamLAND is marked by the ability to detect low-energy anti-neutrino signals at 1,000 tons ofultra pure liquid scintillator (LS) through the inverseβ reaction, 𝜈! + 𝑝 → 𝑒 + 𝑛 . We
demonstrated the oscillation nature of neutrino flavor transformation by observing electron
anti-neutrino (𝜈! ) from nuclear reactors and neutrino properties have been explored precisely[1,2]. Since neutrinos interact with other particles only via weal interaction, they haveextremely low reaction probabilities. Such elusive property of neutrinos provides us with theability to investigate optically invisible deep interior of the astronomical objects, such as the
Earth. Neutrino measurement evolved understanding of neutrino properties to utilization ofneutrino as a “probe”.
The detection of geo-neutrinos, 𝜈! ’s producedin β-decays from primordial radioactivite elements(uranium, thorium and potassium) within thea) Measured geo 𝜈̅! flux at Kamioka and Gran Sasso,
Earth’s interior, brings unique and direct
and expected fluxes at these sites and Hawaii. b)
information about the Earth’s interior and thermal
Measured geo 𝜈̅! flux after subtracting the estimatedcrustal contribution. [4]dynamics.KamLAND detects geo 𝜈! signals above
1.8 MeV due to the reaction threshold energy of the inverse β-decay, resulting to have sensitivity
to 𝜈! ’s from the decay chains of 238U and 232Th. The KamLAND collaboration reported theresult of the first study of geo 𝜈! in 2005 [3]. Later the geo 𝜈! signals at KamLAND wereused to estimate our planet’s radiogenic heat production and constrain composition models of thebulk silicate Earth (BSE) [4]. Following the Fukushima nuclear accident in March 2011, theentire Japanese nuclear reactor industry, which generates >97% of the reactor 𝜈! flux at
KamLAND, has been subjected to a protracted shutdown. This unexpected situation allows us
to improve the sensitivity for geo 𝜈! ’s [5].
Currently, geo 𝜈! observed rate is in agreement with the prediction from existing BSE
composition models within 2σC.L., but some extreme models start to be disfavored. Thisability to discriminate is limited by the experimental uncertainty and crust modeling.
Continuing the data taking under the present low-reactor situation yields better signal-noise ratio
and provides promising power of uncertainty (21%[5] → 15% with 5-year measurement).
Enhanced geo 𝜈! flux calculation model using latest crustal structure model and geochemical
understanding around Japan Island Arc will be a key issue for the further constraint on the Earthmodels and observation of mantle contribution.
The directional measurement of incoming geo 𝜈! ’s can map out the U and Th distribution
inside the Earth and this new technic is also applicable to resolving crust versus mantle flux
contribution. Our experimental studies and Monte-Carlo simulations confirmed that a
combination of 6Li-loaded LS and imaging detector has the feasibility of developing direction
sensitive detector [6]. This new technology will open a new era of understanding of the Earth.
References. [1] Eguchi, K. et al. (2003): Phys. Rev. Lett,90, 021802;[2] Araki, T. et al. (2005): Phys. Rev. Lett, 94,
081801;[3] Araki, T. et al. (2005): Nature, 436, 499; [4] Gando, A. et al. (2011): Nature Geosci, 4, 647; [5] Gando,
A. et al. (2013): Phys. Rev. D, 88, 033001; [6] Tanaka H.K.M and Watanabe H. (2014): Scientific Report (Nature),4, 4708.
54	
  
	
  

	
  

Core and Mantle Compositions: Neutrino Geophysics Insights
W.F. McDonough
Geology, University of Maryland, College Park, MD 20742, USA
Corresponding author’s email address: mcdonoug@umd.edu
The Earth’s four most abundant elements, O, Fe, Mg and Si, make up more than 90% of its
mass; with the addition of Ni, Ca, Al, and S, we describe more than 98% the mass of the planet,
including specifying the core’s and mantle’s compositions. The solar photosphere’s composition
validates the underlying assumption-chondritic meteorites provide a guide to planetary models.
There is no fixed amount of metal accreted or Mg/Si ratio for chondrites. Variations in thisratio reflect the proportion of olivine (2:1 molar Mg/Si) to pyroxene (1:1 molar Mg/Si) accreted
in the planet or chondritic parent body. Astromineralogy studies increasingly reveal variations in
the proportion of olivine to pyroxene in accretion disks, some with inner disk regions richer inolivine relative to the disk wide composition.
Core compositional models remain poorly constrained, with models assuming dissolved O,
Si and S in the Fe-Ni-liquid. However, the relative and absolute abundances of light element(s)in the core remain elusive. There is no compelling reason to have heat producing elements (HPE)in the core; lower limit concentration estimates of HPE in the core are being established.
The upper and lower mantle are regarded as having similar compositions, with seismic
tomography revealing upwelling plumes and downgoing slabs traversing the complete volume of
the mantle, requiring lower-upper mantle mass exchange and mixing. A compositionallyanomalous Earth is no longer tenable given the Earth’s 142Nd-isotopic composition overlaps withthat observed in chondritic meteorites.
The Earth’s geoneutrino signal allows us
to directly assess the amount and distributionof Th and U inside the Earth and define theplanetary budget of these refractory lithophileelements, and hence the amount of Ca and Al
inside the Earth, which in turn defines the
Ca-perovskite content of the lower mantle andfrom that the proportions of bridgmanite andferropericlase [1-3]. Models of SiO2-enrichedlower mantle are disfavored by the recent
geoneutrino result [2], whereas pyrolytic
models and Ca-perovskite-rich models fall within the 1s limits of these results. The lower mantle
has, on average by volume, about 10% Ca-perovskite, 17% ferropericlase, 73% bridgmanite [4].
Variations in the electron density of the Earth’s interior can be probed by neutrino oscillation
studies [5-6] using next-generation detectors. Results from these experiments will evaluate thehydrogen content of the core and later, with increasing data, will test specific compositionalmodels of the relative proportions of O, Si and S dissolved in the metallic liquid alloy. The futureis bright given developments in ocean-going detectors [7] and directionality technology [8];Particle Geoscience will transform our understanding of the Earth’s composition and structure.
References. [1] Usman, S.M. et al. (2015): Scientific Report (Nature), 5,13945; [2] Agostini, M. et al. (2015):
Physical Review D, 92, 031101(R); [3] Gando, A. et al. (2013): Physical Review D, 88, 033001; [4] McDonough,
W.F. (2015): in Deep Earth: Physics and Chemistry of the Lower Mantle and Core (eds., Terasaki, H. & Fischer,R.); [5] Ioannisian, A.N. et al. (2015): Physical Review D, 92, 013014; [6] Rott, C. et al. (2015). [7] Dye, S.et al.
(2015): Physics Procedia, 61, 310-218; [8] Tanaka, H.K.M. and Watanabe, H. (2014): Scientific Report (Nature), 4,
4708.
55