Earth’s Carbon Through Deep Time

Transcript

1. Earth’s Carbon Through Deep Time Robert M. Hazen—Geophysical Lab, Carnegie Institution Goldschmidt Conference, Firenze 29 August 2013
2. DCO website: http://deepcarbon.net •  Begun in 2009 with support from the Sloan Foundation. •  Now into the 5th year of a 10- year program. •  Network of ~1000 collaborators in >40 countries.
3. Cosmic Abundances Carbon is the fourth most abundant element: Sun and Solar System: 23% C (excluding H and He) Carbon in Earth
4. The Carbon Cycle
5. The Deep Carbon Cycle
6. •  What are properties of carbon at extreme pressure and temperature? Questions about Carbon in Earth www.deepcarbon.net!
7. •  What are properties of carbon at extreme pressure and temperature? •  Where is the carbon and how does it move among deep reservoirs and the surface? Questions about Carbon in Earth www.deepcarbon.net!
8. •  What are properties of carbon at extreme pressure and temperature? •  Where is the carbon and how does it move among deep reservoirs and the surface? •  Is there a deep source of organic molecules? Questions about Carbon in Earth www.deepcarbon.net!
9. •  What are properties of carbon at extreme pressure and temperature? •  Where is the carbon and how does it move among deep reservoirs and the surface? •  Is there a deep source of organic molecules? •  What is the nature and extent of deep microbial life? Questions about Carbon in Earth www.deepcarbon.net!
10. www.deepcarbon.net! CARBON IN EARTH!
11. 1.  Origin and evolution of Earth (carbon “mineral evolution”) 2.  Origins and evolution of Life (carbon molecular evolution) 3.  Earth Materials Data Infrastructure EARTH’S CARBON THROUGH DEEP TIME
12. 1.  Origin and evolution of Earth (carbon “mineral evolution”) 2.  Origins and evolution of Life (carbon molecular evolution) 3.  Earth Materials Data Infrastructure EARTH’S CARBON THROUGH DEEP TIME
13. What Is Mineral Evolution? A change over time in: •  The diversity of mineral species •  The relative abundances of minerals •  The compositional ranges of minerals •  The grain sizes and shapes of minerals Hazen et al. (2008) Amer. Mineral. 93, 1693; Hazen et al. (2009) Amer. Mineral. 94, 1293; Hazen et al. (2010) Elements 6, #1, 9-46; Hazen et al. (2011) Amer. Mineral. 96, 953.
14. Mineral Evolution Collaborators Carnegie Institution Xiaoming Liu Anat Shahar Johns Hopkins Univ. Dimitri Sverjensky Charlene Estrada John Ferry Namhey Lee David Azzolini Univ. of Arizona Robert Downs Grethe Hystad Hexiong Yang Joaquin Ruiz Joshua Golden Melissa McMillan Shaunna Morrison Smithsonian Inst. Timothy McCoy Harvard University Andrew Knoll Univ. of Manitoba Andrey Bekker MINDAT.ORG Jolyon Ralph Colorado State Holly Stein Aaron Zimmerman Univ. of Tennessee Linda Kah Boston College Dominic Papineau George Mason Univ. Stephen Elmore Univ. of Maine Edward Grew Indiana University David Bish Univ. of Michigan Rodney Ewing Univ. of Maryland James Farquhar Univ. of Wisconsin John Valley Geol. Survey Canada Wouter Bleeker CalTech Ralph Milliken Rutgers Paul Falkowski
15. Mineral Evolution Collaborators Carnegie Institution Xiaoming Liu Anat Shahar Johns Hopkins Univ. Dimitri Sverjensky Charlene Estrada John Ferry Namhey Lee David Azzolini Univ. of Arizona Robert Downs Grethe Hystad Hexiong Yang Joaquin Ruiz Joshua Golden Melissa McMillan Shaunna Morrison Smithsonian Inst. Timothy McCoy Harvard University Andrew Knoll Univ. of Manitoba Andrey Bekker MINDAT.ORG Jolyon Ralph Colorado State Holly Stein Aaron Zimmerman Univ. of Tennessee Linda Kah Boston College Dominic Papineau George Mason Univ. Stephen Elmore Univ. of Maine Edward Grew Indiana University David Bish Univ. of Michigan Rodney Ewing Univ. of Maryland James Farquhar Univ. of Wisconsin John Valley Geol. Survey Canada Wouter Bleeker CalTech Ralph Milliken Rutgers Paul Falkowski
16. “Ur”-Mineralogy Pre-solar grains contain about a dozen micro- and nano-mineral phases: •  Diamond/Lonsdaleite •  Graphite (C)
17. Diamond & Graphite Graphite Diamond
18. “Ur”-Mineralogy Pre-solar grains contain about a dozen micro- and nano-mineral phases: •  Diamond/Lonsdaleite •  Graphite (C) •  Moissanite (SiC) •  Osbornite (TiN) •  Nierite (Si3 N4 ) •  Rutile (TiO2 ) •  Corundum (Al2 O3 ) •  Spinel (MgAl2 O4 ) •  Hibbonite (CaAl12 O19 ) •  Forsterite (Mg2 SiO4 ) •  Nano-particles of TiC, ZrC, MoC, FeC, Fe-Ni metal within graphite. •  GEMS (silicate glass with embedded metal and sulfide).
19. “Ur”-Mineralogy The earliest mineralogy of the Cosmos was abundant in, if not dominated by, carbon minerals. •  Diamond/Lonsdaleite •  Graphite (C) •  Moissanite (SiC) •  Nano-particles of TiC, ZrC, MoC, FeC
20. Mineral Evolution: How did we get from a dozen minerals to >4800 on Earth today? What does the distribution of carbon minerals through time tell us about key tectonic, geochemical, and biological events?
21. Carbon Allotropes: 4 Carbides: 10 Carbonates: >300 Anhydrous 110 Hydrated ~200 Organic Minerals: ~50 Hydrocarbons 9 Oxalates 12 CARBON MINERALOGY TODAY: 387 IMA approved mineral species
22. Oxidation states from -4 to +4 Bonds to most other elements Most commonly in 2, 3 or 4 coordination CARBON MINERALOGY TODAY: 387 IMA approved mineral species
23. Stage 1: Primary Chondrite Minerals Minerals formed ~4.56 Ga in the Solar nebula “as a consequence of condensation, melt solidification or solid- state recrystallization” (MacPherson 2007) ~60 mineral species •  CAIs •  Chondrules •  Silicate matrix •  Opaque phases
24. Stage 2: Aqueous alteration, metamorphism and differentiation of planetesimals ~250 mineral known species: 4.56-4.55 Ga •  First albite & K-spar •  First significant SiO2 •  Feldspathoids •  Hydrous biopyriboles •  Clay minerals •  Zircon •  Shock phases •  Carbonates
25. Stages 1 and 2: Planetary Accretion ~250 mineral species In these early stages all of Earth’s near-surface compositional complexity was present, but it was not manifest in a diversity of unusual mineral species.
26. Stage 3: Initiation of Igneous Rock Evolution on a Volatile-rich Body (4.55-4.0 Ga) Volcanism, outgasing and surface hydration.
27. Stage 3: Initiation of Igneous Rock Evolution Volatile-rich Body ~30 carbon minerals: Graphite, diamond, lonsdaleite Moissanite, cohenite, haxonite Rhombohedral and orthorhombic carbonates, dominated by Ca, Mg, Fe and possibly Mn
28. Stage 4: Granitoid Formation (>3.5 Ga) >1000 mineral species Partial melting of basalt and/or sediments. (pegmatites)
29. Stage 4: Granitoid Formation (>3.5 Ga) >1000 mineral species Complex pegmatites require multiple cycles of eutectic melting and fluid concentration. (pegmatites) Zabuyelite—Li2 CO3 Niveolanite—NaBeCO3 (OH).2H2 O All known examples are younger than 3.0 Ga.
30. Stage 5: Plate tectonics and large-scale hydrothermal reworking of the crust (>3 Ga) New modes of volcanism Mayon Volcano, Philippines ~108 km3 of reworking
31. Stage 5: Plate tectonics and large-scale hydrothermal reworking of the crust (>3 Ga) Massive base metal deposits (sulfides, sulfosalts) New carbonate sulfates Caledonite Cu2 Pb5 (SO4 )3 (CO3 )(OH)6 Leadhillite Pb4 (CO3 )2 (SO4 )(OH)2 All known examples are younger than 3.0 Ga.
32. Stages 3-5: Era of crust-mantle processing (igneous evolution; plate tectonics) ~1500 mineral New geologic processes, especially fluid- rock interactions associated with igneous activity and plate tectonics, led to a greater diversity of geochemical environments and thus new C mineral species.
33. Stages 3-5: Era of crust-mantle processing (igneous evolution; plate tectonics) ~1500 mineral Nevertheless, we estimate that perhaps only ~75 of the 387 known carbon minerals could have occurred on prebiotic Earth.
34. Stage 6: Anoxic Archean biosphere (3.9-2.5 Ga) ~1,500 mineral species (BIFs, carbonates) Photo credit: D. Papineau Temagami BIFs, ~2.7 Ga Photo credit: F. Corsetti, USC
35. Stage 7: Paleoproterozoic Oxidation (2.5-1.85 Ga) >4,500 mineral species, including perhaps >3,000 new oxides/hydroxides/carbonates Rise of oxygenic photosynthesis. Negaunee BIF, ~1.9 Ga
36. What was the oxygen level in the Archean Eon? log fO2 ~ -72
37. What was the oxygen level in the Archean Eon? Siderite FeCO3 log fO2 < -68
38. What was the oxygen level in the Archean Eon? Azurite & Malachite log fO2 > -43
39. Stage 7: Paleoproterozoic Oxidation (2.5-1.85 Ga) All 369 Cu1+ or Cu2+ + O copper minerals When did these minerals first Azurite Turquoise Dioptase Malachite Chrysocolla
40. Stage 7: Paleoproterozoic Oxidation (2.5-1.85 Ga) Desautelite Mg6 Mn3+ 2 CO3 (OH)16 .4H2 O Pyroaurite Mg6 Fe3+ 2 CO3 (OH)16 .4H2 O What mineral species won’t form? ~220 of 233 U minerals ~400 of 499 Mn minerals >100 of 142 Ni minerals >700 of 1025 Fe minerals Glaucospaerite CuNiCO3 (OH)2 Blatonite UO2 CO3 .H2 O
41. Stages 6-10: Co-evolution of the geosphere and biosphere >4600 mineral Changes in Earth’s atmospheric composition at ~2.4 to 2.2 Ga represent the single most significant factor in our planet’s mineralogical diversity.
42. Stages 6-10: Co-evolution of the geosphere and biosphere >4600 mineral More than 200 carbonate minerals, including >150 hydrous carbonate species, appeared for the first time after the GOE. (Cu, Zn, Ni, Fe3+, Mn4+, U6+)
43. Stage 10: Phanerozoic Biomineralization (<0.542 Ga) >4,800 mineral species (Biominerals, clays)
44. Stage 10: Phanerozoic Biomineralization (<0.542 Ga) >4,800 mineral species
45. Stage 10: Phanerozoic Biomineralization > 50 Organic Mineral Species Abelsonite—NiC31 H32 N4 Evankite—C24 H48 Ravatite—C24 H48 Oxammite—(NH4 )(C2 O4 ).H2 O Dashkovaite—Mg(HCOO)2 .2H2 O
46. Skeletal Biomineralization
47. 1. C has played a central role in cosmic mineralogy since the first ur-mineral. 2. The Great Oxidation Event was the most important factor in C mineral diversification. 3. The biosphere played a key role in the changing chemistry of the exosphere. CONCLUSIONS: Carbon Mineral Evolution
48. 1.  Origin and evolution of Earth (carbon “mineral evolution”) 2.  Origins and evolution of Life (carbon molecular evolution) 3.  Earth Materials Data Infrastructure EARTH’S CARBON THROUGH DEEP TIME
49. Origins of Life Collaborators Carnegie Institution George Cody Cécile Feuille Aravind Asthagiri Dionysis Foustoukos Jim Cleaves Katya Klochko Shuhei Ohara Caroline Jonsson Chris Johnson Jay Brandes Marilyn Fogel Tim Filley George Mason Univ. Harold Morowitz Kim Cone Johns Hopkins Univ. Dimitri Sverjensky Namhey Lee Charlene Estrada Ken Livi Univ. of Washington John Baross UC Santa Cruz David Deamer Univ. of Arizona Robert Downs Hexiong Yang Univ. of Maine Edward Grew George Washington Univ. Glenn Goodfriend
50. Origins of Life Collaborators Carnegie Institution George Cody Cécile Feuille Aravind Asthagiri Dionysis Foustoukos Jim Cleaves Katya Klochko Shuhei Ohara Caroline Jonsson Chris Johnson Jay Brandes Marilyn Fogel Tim Filley George Mason Univ. Harold Morowitz Kim Cone Johns Hopkins Univ. Dimitri Sverjensky Namhey Lee Charlene Estrada Ken Livi Univ. of Washington John Baross UC Santa Cruz David Deamer Univ. of Arizona Robert Downs Hexiong Yang Univ. of Maine Edward Grew George Washington Univ. Glenn Goodfriend
51. Central Assumptions of Origin-of-Life Research The first life forms were carbon-based. Life’s origin was a chemical process that relied on water, air, and rock. The origin of life required a sequence of emergent steps of increasing complexity. [Hazen (2001) Sci. Amer. 284:76; Hazen (2005) Genesis. NAS Press; Hazen & Sverjensky (2010) Origins of Life 11:157; Hazen (2012) Fund. Geobiology 13:315]
52. Geochemical complexities are key to understanding life’s origins: Gradients Cycles Fluxes Interfaces Chemical complexity [Hazen (2001) Sci. Amer. 284:76; Hazen (2005) Genesis. NAS Press; Hazen & Sverjensky (2010) Origins of Life 11:157; Hazen (2012) Fund. Geobiology 13:315]
53. STEP 1: Emergence of Biomolecules The strategy is to use simple molecules to build larger molecules.
54. STEP 1: Emergence of Biomolecules The strategy is to use simple molecules to build larger molecules.
55. STEP 1: Emergence of Biomolecules The strategy is to use simple molecules to build larger molecules.
56. The Miller-Urey Experiment Organic synthesis near the ocean- atmosphere interface.
57. Organic Synthesis in Interstellar “Dense” Molecular Clouds Experiments at NASA Ames simulate this environment.
58. The Hydrothermal Hypothesis A “BLACK SMOKER”
59. Minerals as Catalysts After Jay Brandes et al., 1998 & 1999
64. Carbon-Addition Reactions: Hydrothermal F-T Synthesis (+CH2) •  Reactants: CO2 + H2 + H2 O •  Catalyst: Iron metal •  Conditions: 300o C 500 atm 24 hours [Brandes et al. (1998) Nature 395:365; Cody et al. (2000) Science 289:1337; Cody et al. (2001) GCA 65:3557; Cody et al. (2004) GCA 68:2185]
65. Carbon-Addition Reactions: Hydroformylation (+CO) [Brandes et al. (1998) Nature 395:365; Cody et al. (2000) Science 289:1337; Cody et al. (2001) GCA 65:3557; Cody et al. (2004) GCA
66. Carbon-Addition Reactions: Hydroformylation (+CO) [Brandes et al. (1998) Nature 395:365; Cody et al. (2000) Science 289:1337; Cody et al. (2001) GCA 65:3557; Cody et al. (2004) GCA
67. Carbon-Addition Reactions: Hydroformylation (+CO) [Brandes et al. (1998) Nature 395:365; Cody et al. (2000) Science 289:1337; Cody et al. (2001) GCA 65:3557; Cody et al. (2004) GCA
68. Mineral Catalyzed Carbon-Addition Reactions [Brandes et al. (1998) Nature 395:365; Cody et al. (2000) Science 289:1337; Cody et al. (2001) GCA 65:3557; Cody et al. (2004) GCA 68:2185]
69. STEP 2: The Emergence of Organized Molecular Systems Prebiotic synthesis processes are facile but indiscriminate. Yet a fundamental attribute of life is a high degree of molecular selectivity and organization. What prebiotic processes might have contributed to such selection and organization?
70. Molecular Self-Organization •  Reactants: Pyruvic acid + CO2 + H2 O •  Conditions: 200o C 2,000 atm 2 hours •  Products: A diverse suite of organic molecules [Cody et al. (2000) Science 289:1337; Hazen & Deamer (2007) OOLEB 37:143; Hazen (2005) Genesis. National Acad. Sci. Press]
71. [Cody et al. (2000) Science 289:1337; Hazen & Deamer (2007) OOLEB 37:143; Hazen (2005) Genesis. NAS Press] Self-Assembling Molecules
72. [Cody et al. (2000) Science 289:1337; Hazen & Deamer (2007) OOLEB 37:143; Hazen (2005) Genesis. NAS Press]
73. Biological Homochirality The most challenging aspect of molecular selection is handedness 4 2 C 3 1 (L)-enantiomer 4 2 C 3 1 (R)-enantiomer How did life on Earth become homochiral? Annual sales of chiral pharmaceuticals approaches $200 billion.
74. Alkali Feldspar (110) [Hazen & Sholl (2003) Nature Mater. 2:367; Hazen (2004) Prog. Biol. 11:137; Downs & Hazen (2004) J. Molec. Catalysis 216:273]
75. Diopside – (110) Face [Hazen & Sholl (2003) Nature Mater. 2:367; Hazen (2004) Prog. Biol. 11:137; Downs & Hazen (2004) J. Molec. Catalysis 216:273]
76. Calcite (214) Faces [Hazen & Sholl (2003) Nature Mater. 2:367; Hazen (2004) Prog. Biol. 11:137; Downs & Hazen (2004) J. Molec. Catalysis 216:273]
77. Selection on Mineral Surfaces Mineral surfaces select and concentrate small molecules [Hazen et al. (2001) PNAS 98:5487; Hazen (2006) Amer. Mineral. 91:1715; Asthagiri & Hazen (2006) Molec. Simulation 33:343]
78. (D)-ASP (L)-ASP The most stable configurations found for D- and L- aspartic acid on calcite (214) surface. The D enantiomer is favored by 8 Kcal/mol. Aspartic Acid on Calcite (214) [Hazen et al. (2001) PNAS 98:5487; Hazen (2006) Amer. Mineral. 91:1715; Asthagiri & Hazen (2006) Molec. Simulation 33:343]
79. Adsorption of L-Glu on Rutile solid conc = 20 g/L ; T = 25!C 0 10 20 30 40 50 60 3 4 5 6 7 8 9 10 11 pH Ads (%) [L-Glu] = 0.5 mM (constant) [NaCl]tot 0.01 M 0.05 M 0.1 M 0.3 M 0 10 20 30 40 50 60 70 80 3 4 5 6 7 8 9 10 Ads (%) pH [Glu]tot 0.1 mM 0.5 mM 1 mM 2 mM [NaCl] = 0.1 M (constant) [Jonsson et al. (2009) Langmuir 25, 12127; (2010) GCA 74, 2356]
80. % adsorption 0 5 10 15 20 25 30 35 40 3 4 5 6 7 8 9 10 Chelating “standing up” Chelating - Monodentate “lying down” Glu on Rutile (110) [Sverjensky et al. (2008) EST 42, 6034; Jonsson et al. (2009) Langmuir 25, 12127] pH
81. Studies Interaction of pentose sugars: arabinose, lyxose, xylose and ribose with TiO2 Klochko et al., OOLEB, in revision. Arabinose Xylose Lyxose Ribose
82. Surface complexation models of L-Lysine and L-glutamate on α-TiO2 0 20 40 60 80 100 3 4 5 6 7 8 9 10 % ads. Lysine pH 0.1 mM 0.2 mM L-Lysine on rutile in 0.1 M NaCl 20 g.L-1 ; 18.1 m2. g-1 Lee et al. (2010) Jonsson et al. (2009) 0 20 40 60 80 100 3 4 5 6 7 8 9 10 % ads. Glutamate pH Glu on Rutile Ionic strength = 0.1M 0.1 mM 0.5 mM 1.0 mM 2.0 mM
83. STEP 3: The Emergence of Self- Replicating Molecular Cycles
84. Minerals as Proto-Enzymes After George Cody et al., 2001
85. OH O OH O OH O OH O OH O H3 C OH O H3 C OH O OH O OH O H3 C OH HO O O OH O HO O NH2 OH O OH O Succinic acid + NH 3 + H 2 ± CO2 " ± CO2 " O OH OH O H H H HO OH O H3 C OH O OH OH O O pyruvic Alanine O H H Towards Serine & cysteine + CO 2 + H 2 " To glycine Towards aspartate Pyrimidines & histidine Deep Organic Synthesis and Life Did deep organic synthesis contribute to the origins of life? (Cody et al. 2001, 2004; Cody 2004)
86. 1. Minerals played key roles in life’s origins through catalysis, selection, and concentration of key biomolecules. 2. Minerals may have acted as primitive enzymes in the first self-replicating cycles. CONCLUSIONS: Origins of Life (carbon molecular evolution)
87. 1.  Origin and evolution of Earth (carbon “mineral evolution”) 2.  Origins and evolution of Life (carbon molecular evolution) 3.  Earth Materials Data Infrastructure EARTH’S CARBON THROUGH DEEP TIME
88. Earth Data Collaborators Carnegie Institution Xiaoming Liu Johns Hopkins Univ. Dimitri Sverjensky Charlene Estrada Univ. of Arizona Robert Downs Joshua Golden Joachin Ruiz Mihei Ducea MELTS Mark Ghiorso RPI Peter Fox Frank Spear Lamont-Doherty Kerstin Lehnert Smithsonian Inst. Liz Cottrell MinDat.Org Jolyon Ralph Rutgers Univ. Paul Falkowski Harvard Univ. Andrew Knoll
89. Earth Data Collaborators Carnegie Institution Xiaoming Liu Johns Hopkins Univ. Dimitri Sverjensky Charlene Estrada Univ. of Arizona Robert Downs Joshua Golden Joachin Ruiz Mihei Ducea MELTS Mark Ghiorso RPI Peter Fox Frank Spear Lamont-Doherty Kerstin Lehnert Smithsonian Inst. Liz Cottrell MinDat.Org Jolyon Ralph Rutgers Univ. Paul Falkowski Harvard Univ. Andrew Knoll
90. RRUFF: Manages the outreach of the “official” International Mineralogical Assoc. mineral list. Mindat.org: Mineral species, associations, and locality information EarthChem & PetDB: Rock chemical data At present no open access mineral databases include systematic information on geochronology and chemistry. Mineralogy Data Bases
91. Numerous correlations that reveal aspects of Earth history are hidden in existing data resources. Molybdenite Be-B minerals Hg minerals “Brute Force” Use Cases
92. RESULTS: Molybdenite (MoS2 ) through Time ! Golden et al. (2013) EPSL GOE HERE SE HERE
93. Be Mineral Evolution (Grew & Hazen, 2013)
94. B Mineral Evolution (Grew & Hazen 2010, 2013) Be B
95. Dear Bob, Would it be possible for you to have Shaun Hardy try to obtain the following items through interlibrary loan? The first three papers I tried to get through interlibrary loan at U. Maine, whereas Bob Downs tried to find the fourth item at UA. I need all four for my research on B mineral evolution, and Bob needs the fourth for his research. Avila Salinas W. and Sanjines, O. (1973) Estudio cristalografico y espectrografico de la danburita de Cristal-Mayo (Chapara), Departmento de Cochabamba. Sociedad Geologica Boliviana Boletin, 20, 129-144. Obradovic, J., Karamata, S., Vasic, N., dimitrijevic, R., Milojkovic (1984) Lueneburgite from sedimentary magnesite deposit “Bela Stena” 1 Jugoslav. Simposium za mineralogiju, Arandjelovac 1983, 34-42, Beograd (in Serbian, English summary) Frankl, J. (1959) La ‘Formacion Limbo’. Boletin tecnico de Yacimientos petroliferos fiscales Bolivianos, II, no. 5, 29-38. Avrova, N.P., Bocharov, V.M., Khalturina, I.I., Yunosova, Z.R. (1968) Mineralogy of borates in halogen formations. In: Geology and Exploration of Solid Mineral Deposits of Kazakhstan 1969, 169-173 (in Russian) Many thanks for your help. Best wishes, Ed
96. The Supercontinent Cycle
97. The Supercontinent Cycle SUPERCONTINENT STAGE INTERVAL DURATION Kenorland (Superia) Assembly 2.8-2.5 300 Stable 2.5-2.4 100 Breakup 2.4-2.0 400 Columbia (Nuna) Assembly 2.0-1.8 200 Stable 1.8-1.6 200 Breakup 1.6-1.2 400 Rodinia Assembly 1.2-1.0 200 Stable 1.0-0.75 250 Breakup 0.75-0.6 150 Pannotia Assembly 0.6-0.56 40 Stable 0.56-0.54 20 Breakup 0.54-0.43 110 Pangaea Assembly 0.43-0.25 180 Stable 0.25-0.175 75 Breakup 0.175-present 175
98. The Supercontinent Cycle SUPERCONTINENT STAGE INTERVAL DURATION Kenorland (Superia) Assembly 2.8-2.5 300 Stable 2.5-2.4 100 Breakup 2.4-2.0 400 Columbia (Nuna) Assembly 2.0-1.8 200 Stable 1.8-1.6 200 Breakup 1.6-1.2 400 Rodinia Assembly 1.2-1.0 200 Stable 1.0-0.75 250 Breakup 0.75-0.6 150 Pannotia Assembly 0.6-0.56 40 Stable 0.56-0.54 20 Breakup 0.54-0.43 110 Pangaea Assembly 0.43-0.25 180 Stable 0.25-0.175 75 Breakup 0.175-present 175
99. •  Ocean levels •  Carbonate platforms •  Coastal nutrients •  Ocean/atmosphere chemistry •  Climate •  Continental weathering •  Subduction •  Patterns of volcanism Supercontinents & the C Cycle
100. RESULTS: The Supercontinent CYCLE The distribution of zircon crystals through time correlates with the supercontinent cycle over the past 3 billion years. (Condie & Aster 2010; Hawksworth et al. 2010)
101. RESULTS: Mo Mineral Evolution ! Temporal distribution of molybdenite (MoS2 ) Golden et al. (submitted)
102. B and Be Minerals (Grew & Hazen 2010)
103. Hg Mineral Evolution The distribution of mercury (Hg) minerals through time also correlates with the SC cycle over the past 3 billion years, but there’s a gap during the “boring billion”. Hazen et al. (2012) Amer. Mineral. 97:1013.
104. Phanerozoic Biomineralization and the Terrestrial Biosphere (<542 Ma)
105. Hg Mineral Evolution The distribution of mercury (Hg) minerals through the last 400 million years reflects changes in Earth’s biosphere. Hazen et al. (2012) Amer. Mineral. 97:1013.
106. Hg Mineral Evolution The distribution of mercury (Hg) minerals through the last 400 million years reflects changes in Earth’s biosphere. Hazen et al. (2012) Amer. Mineral. 97:1013.
107. Most of what scientists do is collect data to better understand phenomena that we recognize: Atmospheric oxidation The supercontinent cycle ABDUCTIVE DISCOVERY
108. 1. Large integrated data resources can be explored with multivariate techniques (i.e., principal component analysis). ABDUCTIVE DISCOVERY Search for highly correlated patterns among linear combinations of many different variables.
109. 1. Large integrated data resources can be explored with multivariate techniques (i.e., principal component analysis). 2. We can also implement new visualization strategies. ABDUCTIVE DISCOVERY
110. Genetic structure of selected bird taxa (from Peter Fox)" New Opportunities for Data Visualization
111. types Microbes: Abundance “Skylines” characterize habitats, Sogin et al. New Opportunities for Data Visualization
112. 1. Large integrated data resources can be explored with multivariate techniques (i.e., principal component analysis). 2. We can also implement new visualization strategies. 3. These methods represent a path to discovering what “we don’t know we don’t know.” ABDUCTIVE DISCOVERY
113. 1. Published and “dark” data on Earth materials contain important insights related to the coevolution of the geo- and biospheres. 2. An integrated Earth Materials Data Infrastructure could represent a new kind of open-access scientific “instrument.” CONCLUSIONS: Earth Materials Data Infrastructure
114. •  Near-surface carbon mineralogy has changed through Earth history. •  Earth’s geosphere and biosphere have co-evolved in many ways. •  The Earth Materials Data Infrastructure will be an engine of discovery. CONCLUSIONS: Earth’s Carbon Through Deep Time
115. DCO website: http://deepcarbon.net Thank You!