elasticity of iron-rich silicate in earth’s d” layer · wendy l. mao los alamos national...
TRANSCRIPT
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Wendy L. MaoLos Alamos National Laboratory
Elasticity of iron-rich silicate in Earth’s D” layer
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U Chicago
Andrew Campbell (now at U Maryland)
Dion Heinz
Geophysical Lab
Yingwei Fei
Russell Hemley
Ho-kwang Mao
Jinfu Shu
Argonne National Lab
Yue Meng
Vitali Prakapenka
Guoyin Shen
Wolfgang Sturhahn
Jiyong Zhao
SUNY-Stony Brook
Donald Lindsley
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• New phase in MgSiO3 at approximately D” discontinuity conditions– pv (Pbnm) � ppv (Cmcm)
Tsuchiya et al, EPSL 2004
pv ppv
Post-perovskite
Murakami et al, Science 2004
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Post-perovskite
Tsuchiya et al, EPSL 2004
Sidorin et al, Science 1999
Mantle adiabat
Duffy, Nature 2004
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What about Fe?
• D” is where the liquid Fe outer core meets the crystalline silicate mantle– Fe-rich ppv
– ULVZ
– Seismic anisotropy
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Table
Culet
Gasket Sample chamber
Force
Table
Culet
Gasket Sample chamber
Force
Diamond Anvil Cell
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• Samples– Orthopyroxenes: Fs10 (Mg0.9Fe0.1)SiO3,
Fs20, Fs40, Fs60, Fs80
• Thermal insulation– NaCl, SiO2
• Internal pressure standard– Pt, NaCl
• Gasket– Re, Be + graphite insert
Experimental
gasket sample
Pt
diamond anvil
laser
2θ
x-ray beam
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Synchrotron XRD and laser-heated DAC
13-IDD, GSECARS
Image plate
16-IDB, HPCAT
1800 K
Fs40
130 GPa
• Gasket hole ~ 60 µm (culet =150 µm, bevel diameter = 300 µm) • X-ray beam ~ 6 x 7 µm• Double-sided Nd:YLF laser heating
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W. M
ao et a
l,PNAS 2004
Fs20, M
g0.8 Fe0.2 S
iO3
Azimuth (º)
Diffra
ctio
n a
ng
le (2
θ)
0
10
0
20
0
30
0
68
10
41
21
41
6
ppv 113
ppv 020
ppv 002
ppv 022
ppv 023ppv 131
ppv 004ppv 043
ppv 152,062,200ppv 044
ppv 132
diamond spotsbeam stop holder
56
78
910
1112
1314
1516
1718
1920
2-theta
Relative intensity
NaCl
ppv 020
ppv 002
ppv 113ppv 004
ppv 152,062,200ppv 044
ppv 022
ppv 023ppv 131
ppv 132
Re
Re
NaCl
Pt
En80 138 G
Pa, quenched from
2400 K
NaCl
NaCl
Pt
56
78
910
1112
1314
1516
1718
1920
2-theta
Relative intensity
NaCl
ppv 020
ppv 002
ppv 113ppv 004
ppv 152,062,200ppv 044
ppv 022
ppv 023ppv 131
ppv 132
Re
Re
NaCl
Pt
En80 138 G
Pa, quenched from
2400 K
NaCl
NaCl
Pt
pv+ppv
ppvonly
En80, 113 G
Pa, quenched from
2000 KE
n80, 147 GP
a, quenched from 2400 K
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ppv silicate can take a lot of Fe
Rel
ativ
e in
tens
ity
d-spacing (Å)
Diffraction angle (2θ)
4 3.5 3 2.5 2 1.5 1.3
6 8 10 12 14 16 18 20
Fs40, 141 GPaquenched from 1800 K
b)
Re R
e
ppv
022
ppv
131
ppv
132
ppv
113
ppv
004
*
* **** pp
v15
2,06
2,20
0pp
v04
4
**
ppv
023†
†
†
†
Re
3.5 3 2.5 2 1.5 1.3
6 8 10 12 14 16 18
c)
Fs60, 124 GPaquenched from 1800 K
Re
Re
Pt
Pt
ppv
022
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
*
** * **
ppv
152,
062,
200
ppv
044
**
Re
Au
Fs20, 147 GPaquenched from 2400 K
a)
4 3.5 3 2.5 2 1.5 1.3
NaC
l
δ02
0 ppv
002
*
*pp
v02
2
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
***
*
**
ppv
152,
062,
200
ppv
044
* *
NaC
l
Re R
eP
t NaC
l
5 7 9 11 13 15 17 19
ppv
110
*
d)
Fs80, 142 GPaquenched from 2000 K
6 8 10 12 14 16 18
3.5 3 2.5 2 1.5 1.3
Re
Re
Pt
Pt
Pt
Au
ppv
132
ppv
113
ppv
004
ppv
131
ppv
023
ppv
022
** **
*
*
Rel
ativ
e in
tens
ity
d-spacing (Å)
Diffraction angle (2θ)
4 3.5 3 2.5 2 1.5 1.3
6 8 10 12 14 16 18 20
Fs40, 141 GPaquenched from 1800 K
b)
Re R
e
ppv
022
ppv
131
ppv
132
ppv
113
ppv
004
*
* **** pp
v15
2,06
2,20
0pp
v04
4
**
ppv
023†
†
†
†
Re
3.5 3 2.5 2 1.5 1.3
6 8 10 12 14 16 18
c)
Fs60, 124 GPaquenched from 1800 K
Re
Re
Pt
Pt
ppv
022
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
*
** * **
ppv
152,
062,
200
ppv
044
**
Re
Au
Fs20, 147 GPaquenched from 2400 K
a)
4 3.5 3 2.5 2 1.5 1.3
NaC
l
δ02
0 ppv
002
*
*pp
v02
2
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
***
*
**
ppv
152,
062,
200
ppv
044
* *
NaC
l
Re R
eP
t NaC
l
5 7 9 11 13 15 17 19
ppv
110
*
d)
Fs80, 142 GPaquenched from 2000 K
6 8 10 12 14 16 18
3.5 3 2.5 2 1.5 1.3
Re
Re
Pt
Pt
Pt
Au
ppv
132
ppv
113
ppv
004
ppv
131
ppv
023
ppv
022
** **
*
* ppv only
W. Mao et al, PNAS 2005
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Fe-Mg partitioning: unsettled issue
Murakami et al, GRL 2005
Kobayashi et al, GRL 2006
Andrault et al, JGR 2001
Mao et al, Science 1997
Kessen et al, EPSL 2002 +
mw
silicate
MgFe
MgFeK
)/(
)/(=
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4 6 8 10 12 14 16
ppv
020
ppv
132
ppv
002
ppv
022 pp
v02
3
ppv
131
ppv
113
ppv
004
ppv
152,
062,
200
ppv
044
mw
111
mw
200
mw
220
** **
****
ppv
110
ppv
111
ppv
114
ppv
133
*
***
**
Rel
ativ
e in
tens
ity
Diffraction angle (2θ)
Re
Fa30
4 6 8 10 12 14 16
ppv
020
ppv
132
ppv
002
ppv
022 pp
v02
3
ppv
131
ppv
113
ppv
004
ppv
152,
062,
200
ppv
044
mw
111
mw
200
mw
220
** **
****
ppv
110
ppv
111
ppv
114
ppv
133
*
***
**
Rel
ativ
e in
tens
ity
Diffraction angle (2θ)
Re
Fa30
• Starting composition: Fa30 (Fe0.3Mg0.7)2SiO4, Fa45
• After decompression, recovered mw had lattice constant, a0 = 4.2336 Åwhich corresponds to a composition: Fe0.23Mg0.77O
• For mass balance the ppv phase has a composition: Fe0.37Mg0.63SiO3
• Fe partitions strongly into ppvphase?
120 GPa
Fe-Mg partitioning: unsettled issue
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How does Fe affect VS?
222
3
4
)(
Φ=−=
∂∂−=
υυυρ SP
KV
PVK
7 8 9 10 11 12 13 14 15 16 17 182-theta
Rel
ativ
e co
un
ts
d-spacing (Å)
2.7 2.3 2 1.8 1.6 1.5 1.4 1.3 1.2 1.1
Diffraction angle (2θ)
Rel
ativ
e in
tens
ity
ppv
022
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
ppv
152,
062
ppv
044
ppv
110
ppv
200
ppv
025
ppv
222
ppv
111
ppv
040
ppv
042
ppv
133
ppv
151
ppv
114
Pt
Pt
PtPt
ppv
041
7 8 9 10 11 12 13 14 15 16 17 182-theta
Rel
ativ
e co
un
ts
d-spacing (Å)
2.7 2.3 2 1.8 1.6 1.5 1.4 1.3 1.2 1.1
Diffraction angle (2θ)
Rel
ativ
e in
tens
ity
ppv
022
ppv
023
ppv
131
ppv
132
ppv
113
ppv
004
ppv
152,
062
ppv
044
ppv
110
ppv
200
ppv
025
ppv
222
ppv
111
ppv
040
ppv
042
ppv
133
ppv
151
ppv
114
Pt
Pt
PtPt
ppv
041
W. Mao et al, Science 2006
Fs40 ppv, 140 GPa
116
118
120
122
124
126
120 130 140 150 160 170Pressure (GPa)
Vo
lum
e (A
3)V
olum
e (Å
3 )
Pressure (GPa)
Fs40, ppv
116
118
120
122
124
126
120 130 140 150 160 170Pressure (GPa)
Vo
lum
e (A
3)V
olum
e (Å
3 )
Pressure (GPa)
Fs40, ppv
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Nuclear resonant x-ray spectroscopy (NRXS)
APD
APD HRM M
KBmirrors
x-rays
DAC 150nsec
NRIXS signal
SMS signal
nonmagnetic
magnetic
time
Energy
Inte
nsity
Anti-stokes Stokes
Elastic line
Synchrotron 57Fe Mössbauer spectroscopy
XOR, Sector 3, APS, ANLXOR, Sector 3, APS, ANL
Nuclear resonant inelastic x-ray spectroscopy
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Phonon density of states
ω
g(ω
) de
nsity
of s
tate
s Debye Model
“Real” Crystal
2322
)( ωυπ
ω Vg =
333
213
SpD υυυ+=
0 20 40 60 80 100 120
Fs40, ppv
Energy (meV)
Pho
non
DO
S, g
(E)
0 20 40 60 80 100 120
Fs40, ppv
Energy (meV)
Pho
non
DO
S, g
(E)
D
VP, km/sec VS, km/sec ν PREM, mantle side of CMB 13.72 7.26 0.30 ULVZ (Thorne, JGR 2004) 12.35 5.08 0.40 Fs40 ppv at 130 GPa-300 K 12.72 4.86 0.41 Fs40 ppv at 130 GPa-3000 K 11.91 4.05 0.43
W. Mao et al, Science 2006
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Fe in ULVZ
• Fe-rich ppv has low enough Vs to explain the depression of velocity in ULVZ
• When Fe-poor mantle contacts core, a thin layer of Fe-rich ppvforms
• Mantle convection sweeps the thin layer into a thickened pile to form ULVZ
Outer Core
Fe
D’’Fe-poor ppv
Mantle Upwelling
ULVZFe-rich ppv
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Radial x-ray diffraction
Magnitude of waviness-- deviatoric strain & shear strength
Magnitude dependence on hkl-- elasticity tensor
Intensity vs azimuthal angle -- lattice preferred orientation
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Deformation of a germanate analog
In contrast with phenomenological considerations suggesting (010) as a slip plane, lattice planes near (100) became aligned perpendicular to the compression direction, suggesting that slip on (100) or (110) dominated plastic deformation.
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Elastic anisotropy of silicate ppv at 140 GPa
2θ (deg.)
Azi
mut
hala
ngle
, η(d
eg.)
-150
-100
-50
0
50
100
150
9 10 11 12 13 14 15 16
diamond spot
022
113
004
132
131
023,
130
Pt
040
110
Be
100
Be
002
Be
101
042
022
113
004
132
131
023,
130
Pt
040
110
Be
100
Be
002
Be
101
042
-150
-100
-50
0
50
100
150
9 10 11 12 13 14 15 16
W. Mao et al, in prep.
Fs40
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Determination of single-crystal elasticity tensor
1-3cos2ψ
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
Dev
iato
ricst
rain
(ε ψ
)
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
0.004052.441
0.003222.355
0.004272.032
022 110 040
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
0.003411.821
0.003251.744
0.004291.691
023 131 042
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
1-3cosy2
0.003941.540
0.003391.565
0.003371.527
132 113 004
-0.008
-0.006
-0.004
-0.002
0
0.002
0.004
-2 -1 0 1
G(hkl)R-1 = (3H4 - H 2) s11 + (3K4 - K 2) s22 + (3L4 - L 2) s33 + (6H2K2 + L2 - 1) s12 +
(6H2L2 + K2 - 1) s13 + (6K2L2 + H2 – 1) s23 + 3K2L2 s44+ 3H2L2 s55+ 3H2K2 s66
H = hd/a, K = kd/b, L = ld/c
)()cos31()(
)()()( 2 hklQ
hkld
hkldhkldhkl
P
P ⋅−=−
= ψε ψψ
[Q(hkl)/<Q>] G-1 = α G(hkl)R-1 + (1-α) G-1
αψ
2θ
η
A
q
X
0°
cos ψ = cos η ⋅ cos θ ⋅ sin α – sin θ ⋅ cos α
Formulism from Singh et al J. Appl. Phys., 1998
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Linear compressibilities of ppv at 140 GPa
χa = s11 + s12 + s13
χb = s22 + s12 + s23
χc = s33 + s13 + s23
6.1
6.12
6.14
6.16
6.18
6.2
6.22
6.24
95 105 115 125 135 145
Pressure (GPa)
Latti
ce p
aram
eter
(Å
)
8.12
8.16
8.2
8.24
8.28
8.32
95 105 115 125 135 145
2.45
2.46
2.47
2.48
2.49
2.5
2.51
95 105 115 125 135 145
a
b
c6.1
6.12
6.14
6.16
6.18
6.2
6.22
6.24
95 105 115 125 135 145
Pressure (GPa)
Latti
ce p
aram
eter
(Å
)
8.12
8.16
8.2
8.24
8.28
8.32
95 105 115 125 135 145
2.45
2.46
2.47
2.48
2.49
2.5
2.51
95 105 115 125 135 145
a
b
c
c11 c22 c33 c12 c13 c23 c44 c55 c66
1129 1011 1119 814 722 805 97 124 229
In GPa
W. Mao et al, in prep.
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Iitaka et al, Nature 2004
Tsuchiya et al, GRL 2004
MgSiO3 ppv
Theoretically determined velocity anisotropy
Stackhouse et al, EPSL 2005
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2
4
6
8
10
12
14
0 90 180 270
VS1
VS2
VP
Vel
ocity
(km
/sec
)
Propagation direction
[100] [100][010] [001]
a b c a
2
4
6
8
10
12
14
0 90 180 270
VS1
VS2
VP
Vel
ocity
(km
/sec
)
Propagation direction
[100] [100][010] [001]
a b c a
Fs40ppv
W. Mao et al, in prep.
• Very large azimuthal VS anisotropy, (VS,max - VS,min)/VS,aggregate = 44%
• Small azimuthal VP anisotropy, (VP,max - VP,min)/VP,aggregate = 8%
This implies:
• Seismically observable VS splitting even with the 100 slip plane and low degree of LPO
• No seismically observable VPanisotropy
Possible implications
![Page 24: Elasticity of iron-rich silicate in Earth’s D” layer · Wendy L. Mao Los Alamos National Laboratory Elasticity of iron-rich silicate in Earth’s D” layer. ... 1129 1011 1119](https://reader036.vdocuments.site/reader036/viewer/2022090604/6058481462e718113100af66/html5/thumbnails/24.jpg)
• Clapeyron slope of pv-ppv– Topography of the top of D”
– Double crossing
• Melting of ppv– CMB Temperature
• FTIR and visible spectroscopy– Radiative heat transfer in D”
• Brillouin spectroscopy – Elasticity of low-Fe ppv
• Element partitioning among pv, ppv, mw, and Fe– Geochemistry of D”
Current/Future work in D”
![Page 25: Elasticity of iron-rich silicate in Earth’s D” layer · Wendy L. Mao Los Alamos National Laboratory Elasticity of iron-rich silicate in Earth’s D” layer. ... 1129 1011 1119](https://reader036.vdocuments.site/reader036/viewer/2022090604/6058481462e718113100af66/html5/thumbnails/25.jpg)
![Page 26: Elasticity of iron-rich silicate in Earth’s D” layer · Wendy L. Mao Los Alamos National Laboratory Elasticity of iron-rich silicate in Earth’s D” layer. ... 1129 1011 1119](https://reader036.vdocuments.site/reader036/viewer/2022090604/6058481462e718113100af66/html5/thumbnails/26.jpg)
Fs40ppv
W. Mao et al, in prep.
Experimentally determined velocity anisotropy
c11 c22 c33 c12 c13 c23 c44 c55 c66
1129 1011 1119 814 722 805 97 124 229
Stackhouse et al, GRL 2006
Stackhouse et al, EPSL 2005