Figure of rare earth elemental abundances removed due to copyright restrictions.

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1 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,

2 Given that the r-process nucleosynthetic production ratio for 235 U/ 238 U 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

3 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,

4 No. of 238 U atoms/ U atoms Evolution of galaxy ratio Ratio after first supernova Ratio when earth formed Time after our galaxy formed (Billions of years) No. of 232 Th atoms/ U atoms Evolution of galaxy ratio Ratio after first supernova Ratio when earth formed Time after our galaxy formed (Billions of years) Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 4

5 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,

6 O -2 F -1 Li + Be S -2 Cl -1 Mg 2+ Al 3+ Si 4+ Na Ti 4+ Mn 2+ Fe 2+ K + Ca Fe Rb + Zr Sr Ce 3+ Eu 2+ Lu Eu Th 4+ U Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 6

7 Anion Triangular coordination Tetrahedral coordination 0.15 < R c / R a < < R c / R a < 0.41 A B C Octahedral coordination 0.41 < R c / R a < 0.73 D Cubic coordination R c / R a > 0.73 Cation Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 7

8 Figure of 87 Sr/ 86 Sr vs. 87 Rb/ 86 Sr (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,

9 AAAS. All rights reserved. This content is excluded from our Creative Commons license. For more information, see Source: Amelin, Yuri, Alexander N. Krot, et al. "Lead Isotopic Ages of Chondrules and Calcium-Aluminum-Rich Inclusions." Science 297, no (2002):

10 Figure of 207 Pb/ 204 Pb vs. 206 Pb/ 204 Pb 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,

11 Figure of ( 26 Al/ 27 Al) INI x10-5 and time relative to CAI formation (x10 6 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,

12 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,

13 Figure of 107 Ag/ 109 Ag vs. 108 Pd/ 109 Ag, x10 5 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,

14 High Hf/W silicate earth increased growth of 182 W W/ 183 W Growth Core ratio Chondritic W- Isotopic evolution Undifferentiated solar system objects Time of core formation Bulk Silicate Earth Chondrite Low Hf/W core no increase in 182 W Silicate Earth high Hf/W Core low Hf/W Years after t 0 (Ma) Image by MIT OpenCourseWare. 14

15 Figure of ε 182 of Early Archaean samples and 3.8 billion year igneous mix with inset of ε 182 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,

16 Figure of ε 182 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,

17 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. Rock and metal condense in the hot inner solar system. (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) (D) Solid particles stick togeather. Once larger objects have accreted, they are called planetesimals. T-Tauri phases of the Sun creates large solar wind that ejects gas from between the planets. (E) Large outer planets have sufficient mass to accumulate vast atmosphere including H 2 and He. Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 17

18 Triangulum Galaxy Andromeda Galaxy The Local Group Milky Way Galaxy Milky Way Galaxy Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 18

19 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

20 Earth 0.8 Fe(metal)/Si E H Cosmic abundance Reduction/Oxidation Loss/gain of metal Gain/loss of silicon 0.2 L LL CO/CV CM C 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

21 Figure of ε 182 (Earth) - ε 182 (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,

22 1.2 Ti Mo Zr 1.0 Nd Ba Ce Th La Pr Gd U Ca Yb Cu Nb Er Lu Sr Al Lu Ta Sm Sc Rh Dy Tm W V Tb Re Volitility coefficient Y Os Ir Hf Ru Mg Si Cr Co Pd Fe Pt Au Ni As P Cu O Li Mn Na Cd Sb Sn Ge Ag K Se 0.2 Cs ln Bi F Zn Te Br Cl l S Tl B C H N Volitility order Ga Pb Rb Highly refractories Medium refractories Semi-volatiles Highly volatiles Image by MIT OpenCourseWare. After How to Build a Habitable Planet. 22

23 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,

24 Cumulation% 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 X u Fraction in the core K Mantle X cs Fraction in the core Core Hf Na Lithophile Ti Ca Mg Si Fe W Siderophile and Calcophile Au Xu Fraction in the crust Crust X cs mantle X cs crust 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

25 Nucleosynthesis T N Presolar grains Solar Nebula Condensation t NF Accretion Solar wind Regolith Melting Differentiation Core formation Cosmic rays Meteorite Parent Body T F Impacts Meteoroids on heliocentric orbits T C t F Orbital perturbations t C Collision with Earth T T t T Meteorite in laboratory T L Image by MIT OpenCourseWare. After figure 98 in Heide & Wlotzka, Meteorites. 25

26 Time After Solar System Formation (Myr) ε 182 W Juvinas eucrite Eucrite parent body mantle Mars 0 Earth Two-stage model -2.0 Solar E1 MC E2 system -4.0 Core Iron meteorites encrite parent body core Image by MIT OpenCourseWare. 26

27 Partition model D o Partition coefficient E R o Cation radius Image by MIT OpenCourseWare. 27

28 AAAS. All rights reserved. This content is excluded from our Creative Commons license. For more information, see Source: Blundy, Jon, and Bernard Wood. "Partitioning of Trace Elements between Crystals and Melts." Earth and Planetary Science Letters 210, no. 3 (2003):

29 Courtesy of Mineralogical Society of America. Used with permission. 29

30 MIT OpenCourseWare Marine Isotope Chemistry Fall 2012 For information about citing these materials or our Terms of Use, visit:

Element Cube Project (x2)

Element Cube Project (x2) Background: As a class, we will construct a three dimensional periodic table by each student selecting two elements in which you will need to create an element cube. Helpful Links