Figure of rare earth elemental
abundances removed due to copyright
restrictions.
See figure 3.1 on page 26 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
1
Given that the r-process nucleosynthetic production ratio for
235U/238U
is roughly 1.35 ± 0.3, use the present-day terrestrial
isotope ratio to estimate the “age of the elements” assuming
a one-time production event for these isotopes.
2
Figures of recession velocity vs. distance
removed due to copyright restrictions.
See figure 4.4 on page 50 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
3
No. of 238U atoms/100 235U
atoms
400
Ratio when earth formed
300
Evolution of
galaxy ratio
200
100
0
Ratio after first supernova
0
5
10
15
20
25
Time after our galaxy formed (Billions of years)
No. of 232Th atoms/100 235U
atoms
2000
Evolution of
galaxy ratio
1500
1000
Ratio when earth formed
500
0
Ratio after first supernova
0
5
10
15
20
25
Time after our galaxy formed (Billions of years)
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
4
Figure of uranium and thorium ratios vs.
time and age removed due to copyright
restrictions.
See figure 7.1 on page 81 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
5
Li+
O-2
Be2+
0.92
1.38
1.18
K+
1.31
0.45
Cl-1
S-2
Na+
F-1
Al3+
Mg2+
0.39
Si4+
0.26
1.84
1.81
0.72
Ca2+
1.51
1.00
Rb+
1.61
Sr2+
1.18
Mn2+
Ti4+
0.42
0.66
Fe2+
Fe3+
0.63
0.49
Zr4+
0.59
Ce3+
1.14
Eu2+
1.25
Th4+
U4+
1.05
1.00
Lu3+
Eu3+
1.05
1.06
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
6
Anion
Triangular coordination
Tetrahedral coordination
0.15 < Rc / Ra < 0.22
0.22 < Rc / Ra < 0.41
A
B
C
D
Octahedral coordination
Cubic coordination
0.41 < Rc / Ra < 0.73
Rc / Ra > 0.73
Cation
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
7
Figure of 87Sr/86Sr vs. 87Rb/86Sr (atomic)
removed due to copyright restrictions.
See figure 12.7 on page 179 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
8
© AAAS. All rights reserved. This content is excluded from our Creative Commons
license. For more information, see http://ocw.mit.edu/fairuse.
Source: Amelin, Yuri, Alexander N. Krot, et al. "Lead Isotopic Ages of Chondrules and
Calcium-Aluminum-Rich Inclusions." Science 297, no. 5587 (2002): 1678-83.
9
Figure of 207Pb/204Pb vs. 206Pb/204Pb with
4567 million year reference evolution
line removed due to copyright
restrictions.
See figure 10.3 on page 121 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
10
Figure of (26Al/27Al)INI x10-5 and time
relative to CAI formation (x106 years) vs.
various meteorites removed due to
copyright restrictions.
See figure 11.7 on page 153 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
11
Figure of ages of various meteorites with
respect to solar system formation
removed due to copyright restrictions.
See figure 13.1 on page 193 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
12
Figure of 107Ag/109Ag vs. 108Pd/109Ag, x105
of Gibeon Metal and Normal Silver
removed due to copyright restrictions.
See figure 12.9 on page 182 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
13
High Hf/W silicate earth
increased growth of 182W
c
pi
tion
u
l
o
ev
Undifferentiated solar
system objects
1.85170
0
10
20
30
Time of core formation
W
-I
so
to
Core ratio
Ch
on
dr
iti
c
182
W/183W Growth
1.85205
lk
u
B
th
Ear
e
at
lic
i
S
Chondrite
Low Hf/W core
no increase in 182W
Silicate Earth
high Hf/W
Core
low Hf/W
40
50
Years after t0 (Ma)
Image by MIT OpenCourseWare.
14
Figure of ε182 of Early Archaean samples
and 3.8 billion year igneous mix with
inset of ε182 vs. Cr/Ti for Early Archaean
samples, Enstatite chondrites, Allende
(C1), and Iron meteorites removed due
to copyright restrictions.
See figure 19.1 on page 247 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
15
Figure of ε182 of carbonaceous
chondrites, ordinary chondrites, and iron
meteorites removed due to copyright
restrictions.
See figure 11.8 on page 154 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
16
Rock and metal condense in
the hot inner solar system.
Solar nebula contracts and flattens
into a single spinning disk. The Sun
will form in the center of the disk
containing all the elements, but
mostly h and He.
(A)
H, He and other
noble gases remain
gas. Other elements
condense according
to their volatility.
(B)
Rock, metal and ices
condense in the outer
solar system.
Accretion of planetesi-mals which
will combine in giant impacts
to form the planets.
(C)
T-Tauri phases of the
Sun creates large
solar wind that ejects
gas from between
the planets.
(D)
Solid particles stick togeather.
Once larger objects have
accreted, they are called
planetesimals.
(E)
Large outer planets have
sufficient mass to
accumulate vast
atmosphere including
H2 and He.
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
17
Andromeda
Galaxy
Triangulum
Galaxy
The Local
Group
Milky Way Galaxy
Milky Way Galaxy
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
18
Pluto’s Orbit
Kuiper Belt and outer Solar
System planetary orbits
Orbit of Binary Kulper
Belt Object 1998 WW31
The Oort Cloud
(Comprising many
billions of comets)
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
19
Earth
0.8
os
m
H
ic
”
ab
un
0.4
da
nc
e
Loss/gain of metal
Gain/loss of silicon
“C
0.6
da
xi
O
n/
io
ct
du
Re
Fe(metal)/Si
E
n
tio
L
0.2
CO/CV
LL
CM
0
0
0.2
0.4
0.6
C1
0.8
1.0
Fe(oxide)/Si
Image by MIT OpenCourseWare. After figure 11.1 in Tolstikhin, Igor and Jan Kramers.
"The Evolution of Matter: From the Big Bang to the Present Day."
20
Figure of ε182(Earth) - ε182(initial) vs. time
(millions of years) and
Concentration/concentration in C1 vs.
time (millions of years) removed due to
copyright restrictions.
See figure 18.3 on page 241 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
21
1.2
Ti
Mo
Zr
Pr
1.0
0.8
Volitility coefficient
Nd
Ba
Ce Th
La Yb
Cu Nb
Gd U
Er Lu
Ca Al
Sr
Lu Ta
Rh
Sm Sc
Tm
Dy
W
V
Tb
Y
Re
Hf
Os
Ru
Ir
Mg
Si
Co
Cr
0.6
Fe
Pd
Pt
Ni
Au
P
As
0.4
O
Cu
Mn
Na
Li
Ga
0.2
0
0
10
20
30
40
Cd Sb
Pb Rb K
50
Sn Ge
Cs
Ag
Bi
60
Se ln
F
Zn
Te Br
Cl
l S
Tl
B C
70
H
N
80
Volitility order
Highly refractories
Medium refractories
Semi-volatiles
Highly volatiles
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
22
Figure of Depletion relative to C1 and
refractory element vs. Increasing
siderophile behavior of refractory and
transitional elements and volatile
elements and low-pressure metal-silicate
partition coefficients removed due to
copyright restrictions.
See figure 18.1 on page 232 of Tolstikhin,
Igor and Jan Kramers. “The Evolution of
Matter: From the Big Bang to the Present
Day.” Cambridge University Press, 2008.
23
Cumulation%
0
Rb
Ba
K
B
Be
Pr
Sr
Hf
Nb
Sm
Eu
Tb
In
Er
Lu
Tm
Ti
Ca
O
Mg
Si
V
Cs
Cd
Cu
TI
I
Fe
W
Ag
P
N
As
Se
Re
Ru
Ir
0.1
0.2 0.3
0.4
0.5 0.6
Xu Fraction in the core
0.7 0.8 0.9
Xu Fraction in the crust
Crust
K
Hf
Na
Lithophile
Mantle
Ti
Ca
Mg
Si
Xcs Fraction in the core
Xcs mantle
Fe
Core
W
Siderophile and Calcophile
Au
Xcs crust
1
Th
U
F
La
Ce
Ta
Nd
Zr
Li
Na
Gd
Dy
Ho
Y
Yb
Ga
AI
Sc
Zn
Co
Mn
Pb
Cr
Sn
Hg
Bi
CI
Br
Ge
Sb
Ni
S
Mo
Au
Pd
Pt
Os
Image by MIT OpenCourseWare. After How to Build a Habitable Planet.
24
TN
Nucleosynthesis
Presolar grains
Solar Nebula
∆tNF
Condensation
Accretion
Solar wind
Regolith
Melting
Differentiation
Core formation
Meteorite
Parent
Body
Cosmic rays
TF
Impacts
Meteoroids
on heliocentric
orbits
TC
tC
Orbital perturbations
Collision with Earth
tF
TT
tT
Meteorite in laboratory
TL
Image by MIT OpenCourseWare. After figure 98 in Heide & Wlotzka, Meteorites.
25
Time After Solar System Formation (Myr)
ε182W
+10.0
Juvinas
eucrite
+8.0
Eucrite parent
body mantle
+6.0
+4.0
+2.0
Mars
0
Earth
-2.0
Two-stage model
Solar
system
E1
Iron meteorites
encrite parent body core
Core
-4.0
0
10
E2
MC
20
30
40
50
60
Image by MIT OpenCourseWare.
26
Partition model
Partition coefficient
Do
Ro
E
Cation radius
Image by MIT OpenCourseWare.
27
© AAAS. All rights reserved. This content is excluded from our Creative Commons
license. For more information, see http://ocw.mit.edu/fairuse.
Source: Blundy, Jon, and Bernard Wood. "Partitioning of Trace Elements between Crystals
and Melts." Earth and Planetary Science Letters 210, no. 3 (2003): 383-97.
28
Courtesy of Mineralogical Society of America. Used with permission.
29
MIT OpenCourseWare
http://ocw.mit.edu
12.744 Marine Isotope Chemistry
Fall 2012
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