Today s topic: co evolution of Earth & life
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1 Co evolution of the atmosphere, oceans, and life of Earth Yasuhito SEKINE Dept. Complexity Si& Sci. Engr. The University of Tokyo Habitable planet workshop
2 Today s topic: co evolution of Earth & life Figure after TPF HP Earth is the only known aqua planet so far. We need to know how the ocean, atmosphere, and life have evolved and interacted over Earth s history.
3 Evolution of Earth s atmosphere Log (partial pressures s) (bar) 11 O CH 4 N Age (billion years ago) CO 2 (Holland, 1984; Tajika & Matsui, 1992; Kasting, 1993; Rye & Holland, 1998; Farquhar et al., 2; Pavlov et al., 21; Hoffman & Schrag, 2; Zahnle et al., 26)
4 Evolution of Earth s atmosphere Log (partial pressures s) (bar) Cyanobacteria (O 2 producing N 2 bacteria) 1 O CH 4 Phytoplankton 4 (Eukaryotes) 3. Mth Methanogen (CH 4 producing CO 2 bacteria) Age (billion years ago) (Holland, 1984; Tajika & Matsui, 1992; Kasting, 1993; Rye & Holland, 1998; Farquhar et al., 2; Pavlov et al., 21; Hoffman & Schrag, 2; Zahnle et al., 26)
5 Log (partial pressures s) (bar) Evolution of Earth s atmosphere Q1. How had the early Earth been The Great seen Oxidation from space? Event: the most sg significant tchemical ca transition ta sto N 2 Q2. Why did the O 2 levels l rise at the time? Cyanobacteria is considered to have evolved at least 2.7 billion years ago (Brocks et al., 1999) CH 4 O 2 CO 2 4 Q3. Why did the increase in O 2 occur so Age (billion years ago) rapidly in geological g timescale? (Holland, 1984; Tajika & Matsui, 1992; Kasting, 1993; Rye & Holland, 1998; Farquhar et al., 2; Pavlov et al., 21; Hoffman & Schrag, 2; Zahnle et al., 26)
6 Q1. How had the early Earth been seen from space? Key: Titan (Organic chemistry in CH 4 rich c atmosphere) e) N 2 CH 4 H C 2 H 2 C 4 H 2 HCN H Titan atmosphere N 2 : 95 98%, CH 4 : 2 5% Organic aerosols
7 Q1. How had the early Earth been seen from space? Key: Titan (Organic chemistry in CH 4 rich c atmosphere) e) Titan aerosol analog (tholin) Formed from N 2 /CH 4 =9/1 gas mixtures Titan atmosphere N 2 : 95 98%, CH 4 : 2 5%
8 Time Orange early Earth? Atmospheric composition O 2 N 2 Oxidizing Aerosol formed from N 2 /CH 4 = 9/1 CH 4 + 3O CO + 2H 2 O 4 2 Planetary CO 2 N 2 CH 4 /CO 2 >.5 (Trainer et al., 27) 4 2 CO 2 + CH 4 N 2 Range for aerosol mass Laboratory experiments are key to predict the H 2 formation surface environment of Super Earths. Aerosol formed from H 2 /CH 4 = 1/1 H 2 CH 4 CH4 /H 2 >.5? (Khare et al., 1984) H 2 He + CH 4 + NH 3 C 2 H 2 + 6H 2CH 4 Reducing Black Super Earths?
9 Q2. Why billion years ago? Key: Ocean composition (A decline in Ni abundance in the oceans from 2.5 billion years ago) (Konhauser et al., 29) Cooling Earth s mantle and a decrease in eruption deposits of Ni rich volcanic rocks. Ni/Fe Molar High Ni abundance in the oceans Oceanic Ni depletion Ancient marine sediments (Banded iron formations) Age (billion years ago)
10 Q2. Why billion years ago? Key: Ocean composition (A decline in Ni abundance in the oceans from 2.5 billion years ago) (Konhauser et al., 29) Ni is an bioessential element for methanogen Ni/Fe Molar High Ni abundance in the oceans An enzyme of methanogen Oceanic Ni depletion Thermal evolution & a decline in Ni in the oceans a methanogen famine & an increase in O 2. Age (billion years ago) Ni +
11 Q3. Why did O 2 increase so rapidly? Key: Climate change (A decline in CH 4 severe ice age) Log (pa rtial pres ssures) (b bar) TheGreat Oxidation Event O 2 N 2 Glaciations (Huronian glaciation) i CO 2 44 CH 4 How were the severe glaciations related with the increase in O 2 levels? Timing is everything! Age (billion years ago)
12 Osmium (Os) isotopic compositions in ancient oceans (Sekine et al., under review) Point 1: Continental crusts have high concentrations of 187 Os decayed from 187 Re contained in continents. 192 Os 19 Os 189 Os 188 Os 187 Os β decay (λ=1.66x1-11 ) 187 Re Point 2: Os is a redox sensitive element, soluble and mobile in hydrological cycle only under oxidizing atmospheres Reducing Oxidizing Os (immobile) HOsO 5 (mobile)
13 Osmium (Os) isotopic compositions in ancient oceans (Sekine et al., under review) Oidii Oxidizing atmospheres seawater 187 O/ Os/ 188 Os > Reducing atmospheres seawater 187 Os/ 188 Os ~ Continental (radiogenic) Os No input 187 Os/ 188 Os 1.4 (high) Hydrothermal activities Mantle derived Os 187 Os/ 188 Os.12 (low) Current seawater Os 187 Os/ 188 Os 1.6 Oxidative weathering (Peucker Ehrenbrink & Ravizza, 2)
14 Huronian Supergroup (Canada) 2.22 billion years ago Climatic cycles Interglacial Gowganda fm Glaciation Interglacial Bruce fm Glaciation carbonate glacial diamictite sandstone mudstone volcanic rock Ramsey lake fm 2.45 billion years ago Interglacial Glaciation
15 Variation in initial 187 Os/ 188 Os (age =2.3±.2 Ga) Sandstone siltstone interval (greenhouse) Recording a climatic recovery Glacial diamictite (ice house) Mantle derived value at 2.3 Ga
16 Variation in initial 187 Os/ 188 Os (age =2.3±.2 Ga) Increasing radiogenic Os The synchronicity of an episode of increasing O 2 and deglaciation. An increase in the input of radiogenic continental t Os Climatic recovery acted to accelerate No the input rise in of O 2 (by providing continental nutrients (phosphate) for Mantle derived value at 2.3 Ga cyanobacteria?) (Kirschvink et al., 2; Sekine et al., under review). radiogenic Os
17 Relationship between climate & O 2 Cyanobacteria blooming O 2 increase Glaciation Atmospheric reactions Mitigating the greenhouse effect CH 4 decline N A positive feedback: A driving force for 2 the rapid & irreversible Glaciations transitiontoto the oxidizing world (partial pressures s) (bar) 11 Glaciations 22 3 CH 4 O 2 CO 2 Log Age (billion years ago)
18 In the aftermath of the rise in O 2 Enhancements of other redox sensitive metals Mo, Zn, & V in oceans, bioessential element for Eukaryotes (Anbar & Knoll, 22; Knoll et al., 26; Dupont et al., 26) leading to prosperity of Eukaryotes (partial pressures s) (bar) CH 4 Eukaryote Bacteria & Achaea O 2 N 2 CO 2 Animals Log Age (billion years ago)
19 Summary In Earth s history, the evolutions of the atmosphere, ocean, and climate have been closely related with that of life. Log (partial pressures s) (bar) 11 N Change in volcanic rocks (Ni poor rocks) N 2 Methanogen famine & decline in CH 4 Climatic change: Glaciation interglaciationinterglaciation 22 O 2 3 CH Supply of nutrients for cyanobacteria & the rise in O CO 2 The prosperity of Eukaryotes (including us) Age (billion years ago)
20 Summary Earth is, probably, not the only aqua planet. 21 s: Sizes & densities of Earths Kepler mission (NASA) How many Earths are in our galaxy? 22 s: Atmospheres of Earths Darwin mission (ESA) Terrestrial Planet Finder (NASA) How many Earths have oxidizing atmospheres? How many reducing atmospheres? Or, something else?
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