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Great Oxidation Event

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For the second (Neoproterozoic) surge in atmospheric oxygen, see Neoproterozoic oxygenation event.

Timescale
O2 build-up in the Earth's atmosphere. Red and green lines represent the range of the estimates while time is measured in billions of years ago (Ga).
  • Stage 1 (3.85–2.45 Ga): Practically no O2 in the atmosphere. The oceans were also largely anoxic – with the possible exception of O2 in the shallow oceans.
  • Stage 2 (2.45–1.85 Ga): O2 produced, rising to values of 0.02 and 0.04 atm, but absorbed in oceans and seabed rock.
  • Stage 3 (1.85–0.85 Ga): O2 starts to gas out of the oceans, but is absorbed by land surfaces. No significant change in oxygen level.
  • Stages 4 and 5 (0.85 Ga – present): Other O2 reservoirs filled; gas accumulates in atmosphere.[1]

The Great Oxidation Event (GOE) or Great Oxygenation Event, also called the Oxygen Catastrophe, Oxygen Revolution, Oxygen Crisis or Oxygen Holocaust,[2] was a time interval during the Earth's Paleoproterozoic era when the Earth's atmosphere and shallow seas first experienced a rise in the concentration of free oxygen.[3] This began approximately 2.460–2.426 Ga (billion years) ago during the Siderian period and ended approximately 2.060 Ga ago during the Rhyacian.[4] Geological, isotopic and chemical evidence suggests that biologically produced molecular oxygen (dioxygen or O2) started to accumulate in the Archean prebiotic atmosphere due to microbial photosynthesis, and eventually changed it from a weakly reducing atmosphere practically devoid of oxygen into an oxidizing one containing abundant free oxygen,[5] with oxygen levels being as high as 10% of modern atmospheric level by the end of the GOE.[6]

The appearance of highly reactive free oxygen, which can oxidize organic compounds (especially genetic materials) and thus is toxic to the then-mostly anaerobic biosphere, may have caused the extinction/extirpation of many early organisms on Earth – mostly archaeal colonies that used retinal to use green-spectrum light energy and power a form of anoxygenic photosynthesis (see Purple Earth hypothesis). Although the event is inferred to have constituted a mass extinction,[7] due in part to the great difficulty in surveying microscopic organisms' abundances, and in part to the extreme age of fossil remains from that time, the Great Oxidation Event is typically not counted among conventional lists of "great extinctions", which are implicitly limited to the Phanerozoic eon. In any case, isotope geochemistry data from sulfate minerals have been interpreted to indicate a decrease in the size of the biosphere of >80% associated with changes in nutrient supplies at the end of the GOE.[8]

The GOE is inferred to have been caused by cyanobacteria, which evolved chlorophyll-based photosynthesis that releases dioxygen as a byproduct of water photolysis. The continually produced oxygen eventually depleted all the surface reducing capacity from ferrous iron, sulfur, hydrogen sulfide and atmospheric methane over nearly a billion years. The oxidative environmental change, compounded by a global glaciation, devastated the microbial mats around the Earth's surface. The subsequent adaptation of surviving archaea via symbiogenesis with aerobic proteobacteria (which went endosymbiont and became mitochondria) may have led to the rise of eukaryotic organisms and the subsequent evolution of multicellular life-forms.[9][10][11]

Early atmosphere

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Main articles: Paleoatmosphere and Prebiotic atmosphere
See also: Paleoclimatology and Atmosphere of Earth

The composition of the Earth's earliest atmosphere is not known with certainty. However, the bulk was likely nitrogen N2, and carbon dioxide CO2, which are also the predominant nitrogen- and carbon-bearing gases produced by volcanism today. These are relatively inert gases. Oxygen, O2, meanwhile, was present in the atmosphere at just 0.001% of its present atmospheric level.[12][13] The Sun shone at about 70% of its current brightness 4 billion years ago, but there is strong evidence that liquid water existed on Earth at the time. A warm Earth, in spite of a faint Sun, is known as the faint young Sun paradox.[14] Either CO2 levels were much higher at the time, providing enough of a greenhouse effect to warm the Earth, or other greenhouse gases were present. The most likely such gas is methane, CH
4, which is a powerful greenhouse gas and was produced by early forms of life known as methanogens. Scientists continue to research how the Earth was warmed before life arose.[15]

An atmosphere of N2 and CO2 with trace amounts of H2O, CH4, carbon monoxide (CO), and hydrogen (H2) is described as a weakly reducing atmosphere.[16] Such an atmosphere contains practically no oxygen. The modern atmosphere contains abundant oxygen (nearly 21%), making it an oxidizing atmosphere.[17] The rise in oxygen is attributed to photosynthesis by cyanobacteria, which are thought to have evolved as early as 3.5 billion years ago.[18]

The current scientific understanding of when and how the Earth's atmosphere changed from a weakly reducing to a strongly oxidizing atmosphere largely began with the work of the American geologist Preston Cloud in the 1970s.[14] Cloud observed that detrital sediments older than about 2 billion years contained grains of pyrite, uraninite,[14] and siderite,[17] all minerals containing reduced forms of iron or uranium that are not found in younger sediments because they are rapidly oxidized in an oxidizing atmosphere. He further observed that continental red beds, which get their color from the oxidized (ferric) mineral hematite, began to appear in the geological record at about this time. Banded iron formation largely disappears from the geological record at 1.85 Ga, after peaking at about 2.5 Ga.[19] Banded iron formation can form only when abundant dissolved ferrous iron is transported into depositional basins, and an oxygenated ocean blocks such transport by oxidizing the iron to form insoluble ferric iron compounds.[20] The end of the deposition of banded iron formation at 1.85 Ga is therefore interpreted as marking the oxygenation of the deep ocean.[14] Heinrich Holland further elaborated these ideas through the 1980s, placing the main time interval of oxygenation between 2.2 and 1.9 Ga.[15]

Constraining the onset of atmospheric oxygenation has proven particularly challenging for geologists and geochemists. While there is a widespread consensus that initial oxygenation of the atmosphere happened sometime during the first half of the Paleoproterozoic, there is disagreement on the exact timing of this event. Scientific publications between 2016–2022 have differed in the inferred timing of the onset of atmospheric oxygenation by approximately 500 million years; estimates of 2.7 Ga,[21] 2.501–2.434 Ga[22] 2.501–2.225 Ga,[23] 2.460–2.426 Ga,[4] 2.430 Ga,[24] 2.33 Ga,[25] and 2.3 Ga have been given.[26] Factors limiting calculations include an incomplete sedimentary record for the Paleoproterozoic (e.g., because of subduction and metamorphism), uncertainties in depositional ages for many ancient sedimentary units, and uncertainties related to the interpretation of different geological/geochemical proxies. While the effects of an incomplete geological record have been discussed and quantified in the field of paleontology for several decades, particularly with respect to the evolution and extinction of organisms (the Signor–Lipps effect), this is rarely quantified when considering geochemical records and may therefore lead to uncertainties for scientists studying the timing of atmospheric oxygenation.[23]

Geological evidence

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Evidence for the Great Oxidation Event is provided by a variety of petrological and geochemical markers that define this geological event.

Continental indicators

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Paleosols, detrital grains, and red beds are evidence of low oxygen levels.[27] Paleosols (fossil soils) older than 2.4 billion years old have low iron concentrations that suggest anoxic weathering.[28] Detrital grains composed of pyrite, siderite, and uraninite (redox-sensitive detrital minerals) are found in sediments older than ca. 2.4 Ga.[29] These minerals are only stable under low oxygen conditions, and so their occurrence as detrital minerals in fluvial and deltaic sediments are widely interpreted as evidence of an anoxic atmosphere.[29][30] In contrast to redox-sensitive detrital minerals are red beds, red-colored sandstones that are coated with hematite. The occurrence of red beds indicates that there was sufficient oxygen to oxidize iron to its ferric state, and these represent a marked contrast to sandstones deposited under anoxic conditions which are often beige, white, grey, or green.[31]

Banded iron formation

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Banded iron formations are composed of thin alternating layers of chert (a fine-grained form of silica) and iron oxides (magnetite and hematite). Extensive deposits of this rock type are found around the world, almost all of which are more than 1.85 billion years old and most of which were deposited around 2.5 Ga. The iron in banded iron formations is partially oxidized, with roughly equal amounts of ferrous and ferric iron.[32] Deposition of a banded iron formation requires both an anoxic deep ocean capable of transporting iron in soluble ferrous form, and an oxidized shallow ocean where the ferrous iron is oxidized to insoluble ferric iron and precipitates onto the ocean floor.[20] The deposition of banded iron formations before 1.8 Ga suggests the ocean was in a persistent ferruginous state, but deposition was episodic and there may have been significant intervals of euxinia.[33] The transition from deposition of banded iron formations to manganese oxides in some strata has been considered a key tipping point in the timing of the GOE because it is believed to indicate the escape of significant molecular oxygen into the atmosphere in the absence of ferrous iron as a reducing agent.[34]

Iron speciation

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Black laminated shales, rich in organic matter, are often regarded as a marker for anoxic conditions. However, the deposition of abundant organic matter is not a sure indication of anoxia, and burrowing organisms that destroy lamination had not yet evolved during the time frame of the Great Oxygenation Event. Thus laminated black shale by itself is a poor indicator of oxygen levels. Scientists must look instead for geochemical evidence of anoxic conditions. These include ferruginous anoxia, in which dissolved ferrous iron is abundant, and euxinia, in which hydrogen sulfide is present in the water.[35]

Examples of such indicators of anoxic conditions include the degree of pyritization (DOP), which is the ratio of iron present as pyrite to the total reactive iron. Reactive iron, in turn, is defined as iron found in oxides and oxyhydroxides, carbonates, and reduced sulfur minerals such as pyrites, in contrast with iron tightly bound in silicate minerals.[36] A DOP near zero indicates oxidizing conditions, while a DOP near 1 indicates euxinic conditions. Values of 0.3 to 0.5 are transitional, suggesting anoxic bottom mud under an oxygenated ocean. Studies of the Black Sea, which is considered a modern model for ancient anoxic ocean basins, indicate that high DOP, a high ratio of reactive iron to total iron, and a high ratio of total iron to aluminum are all indicators of transport of iron into a euxinic environment. Ferruginous anoxic conditions can be distinguished from euxenic conditions by a DOP less than about 0.7.[35]

The currently available evidence suggests that the deep ocean remained anoxic and ferruginous as late as 580 Ma, well after the Great Oxygenation Event, remaining just short of euxenic during much of this interval of time. Deposition of banded iron formation ceased when conditions of local euxenia on continental platforms and shelves began precipitating iron out of upwelling ferruginous water as pyrite.[33][27][35]

Isotopes

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Some of the most persuasive evidence for the Great Oxidation Event is provided by the mass-independent fractionation (MIF) of sulfur. The chemical signature of the MIF of sulfur is found prior to 2.4–2.3 Ga but disappears thereafter.[37] The presence of this signature all but eliminates the possibility of an oxygenated atmosphere.[17]

Different isotopes of a chemical element have slightly different atomic masses. Most of the differences in geochemistry between isotopes of the same element scale with this mass difference. These include small differences in molecular velocities and diffusion rates, which are described as mass-dependent fractionation processes. By contrast, MIF describes processes that are not proportional to the difference in mass between isotopes. The only such process likely to be significant in the geochemistry of sulfur is photodissociation. This is the process in which a molecule containing sulfur is broken up by solar ultraviolet (UV) radiation. The presence of a clear MIF signature for sulfur prior to 2.4 Ga shows that UV radiation was penetrating deep into the Earth's atmosphere. This in turn rules out an atmosphere containing more than traces of oxygen, which would have produced an ozone layer that would have shielded the lower atmosphere from UV radiation. The disappearance of the MIF signature for sulfur indicates the formation of such an ozone shield as oxygen began to accumulate in the atmosphere.[17][27] MIF of sulphur also indicates the presence of oxygen in that oxygen is required to facilitate repeated redox cycling of sulphur.[38]

MIF provides clues to the Great Oxygenation Event. For example, oxidation of manganese in surface rocks by atmospheric oxygen leads to further reactions that oxidize chromium. The heavier 53Cr is oxidized preferentially over the lighter 52Cr, and the soluble oxidized chromium carried into the ocean shows this enhancement of the heavier isotope. The chromium isotope ratio in banded iron formation suggests small but significant quantities of oxygen in the atmosphere before the Great Oxidation Event, and a brief return to low oxygen abundance 500 Ma after the GOE. However, the chromium data may conflict with the sulfur isotope data, which calls the reliability of the chromium data into question.[39][40] It is also possible that oxygen was present earlier only in localized "oxygen oases".[41] Since chromium is not easily dissolved, its release from rocks requires the presence of a powerful acid such as sulfuric acid (H2SO4) which may have formed through bacterial oxidation of pyrite. This could provide some of the earliest evidence of oxygen-breathing life on land surfaces.[42]

Other elements whose MIF may provide clues to the GOE include carbon, nitrogen, transitional metals such as molybdenum and iron, and non-metal elements such as selenium.[27]

Fossils and biomarkers

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See also: Biomarker (petroleum)

While the GOE is generally thought to be a result of oxygenic photosynthesis by ancestral cyanobacteria, the presence of cyanobacteria in the Archaean before the GOE is a highly controversial topic.[43] Structures that are claimed to be fossils of cyanobacteria exist in rock formed 3.5 Ga.[44] These include microfossils of supposedly cyanobacterial cells and macrofossils called stromatolites, which are interpreted as colonies of microbes, including cyanobacteria, with characteristic layered structures. Modern stromatolites, which can only be seen in harsh environments such as Shark Bay in Western Australia, are associated with cyanobacteria, and thus fossil stromatolites had long been interpreted as the evidence for cyanobacteria.[44] However, it has increasingly been inferred that at least some of these Archaean fossils were generated abiotically or produced by non-cyanobacterial phototrophic bacteria.[45]

Additionally, Archaean sedimentary rocks were once found to contain biomarkers, also known as chemical fossils, interpreted as fossilized membrane lipids from cyanobacteria and eukaryotes. For example, traces of 2α-methylhopanes and steranes that are thought to be derived from cyanobacteria and eukaryotes, respectively, were found in the Pilbara of Western Australia.[46] Steranes are diagenetic products of sterols, which are biosynthesized using molecular oxygen. Thus, steranes can additionally serve as an indicator of oxygen in the atmosphere. However, these biomarker samples have since been shown to have been contaminated, and so the results are no longer accepted.[47]

Carbonaceous microfossils from the Turee Creek Group of Western Australia, which date back to ~2.45–2.21 Ga, have been interpreted as iron-oxidising bacteria. Their presence suggests a minimum threshold of seawater oxygen content had been reached by this interval of time.[48]

Other indicators

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Some elements in marine sediments are sensitive to different levels of oxygen in the environment such as the transition metals molybdenum[35] and rhenium.[49] Non-metal elements such as selenium and iodine are also indicators of oxygen levels.[50]

Hypotheses

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See also: Oxygen cycle

The ability to generate oxygen via photosynthesis likely first appeared in the ancestors of cyanobacteria.[51] These organisms evolved at least 2.45–2.32 Ga[52][53] and probably as early as 2.7 Ga or earlier.[14][54][3][55][56] However, oxygen remained scarce in the atmosphere until around 2.0 Ga,[15] and banded iron formation continued to be deposited until around 1.85 Ga.[14] Given the rapid multiplication rate of cyanobacteria under ideal conditions, an explanation is needed for the delay of at least 400 million years between the evolution of oxygen-producing photosynthesis and the appearance of significant oxygen in the atmosphere.[15]

Hypotheses to explain this gap must take into consideration the balance between oxygen sources and oxygen sinks. Oxygenic photosynthesis produces organic carbon that must be segregated from oxygen to allow oxygen accumulation in the surface environment, otherwise the oxygen back-reacts with the organic carbon and does not accumulate. The burial of organic carbon, sulfide, and minerals containing ferrous iron (Fe2+) is a primary factor in oxygen accumulation.[57] When organic carbon is buried without being oxidized, the oxygen is left in the atmosphere. In total, the burial of organic carbon and pyrite today creates 15.8±3.3 Tmol (1 Tmol = 1012 moles) of O2 per year. This creates a net O2 flux from the global oxygen sources.

The rate of change of oxygen can be calculated from the difference between global sources and sinks.[27] The oxygen sinks include reduced gases and minerals from volcanoes, metamorphism and weathering.[27] The GOE started after these oxygen-sink fluxes and reduced-gas fluxes were exceeded by the flux of O2 associated with the burial of reductants, such as organic carbon.[58] About 12.0±3.3 Tmol of O2 per year today goes to the sinks composed of reduced minerals and gases from volcanoes, metamorphism, percolating seawater and heat vents from the seafloor.[27] On the other hand, 5.7±1.2 Tmol of O2 per year today oxidizes reduced gases in the atmosphere through photochemical reaction.[27] On the early Earth, there was visibly very little oxidative weathering of continents (e.g., a lack of red beds), and so the weathering sink on oxygen would have been negligible compared to that from reduced gases and dissolved iron in oceans.

Dissolved iron in oceans exemplifies O2 sinks. Free oxygen produced during this time was chemically captured by dissolved iron, converting iron Fe and Fe2+ to magnetite (Fe2+Fe3+2O4) that is insoluble in water, and sank to the bottom of the shallow seas to create banded iron formations.[58] It took 50 million years or longer to deplete the oxygen sinks.[59] The rate of photosynthesis and associated rate of organic burial also affect the rate of oxygen accumulation. When land plants spread over the continents in the Devonian, more organic carbon was buried and likely allowed higher O2 levels to occur.[60] Today, the average time that an O2 molecule spends in the air before it is consumed by geological sinks is about 2 million years.[61] That residence time is relatively short in geologic time; so in the Phanerozoic, there must have been feedback processes that kept the atmospheric O2 level within bounds suitable for animal life.

Evolution by stages

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Preston Cloud originally proposed that the first cyanobacteria had evolved the capacity to carry out oxygen-producing photosynthesis but had not yet evolved enzymes (such as superoxide dismutase) for living in an oxygenated environment. These cyanobacteria would have been protected from their own poisonous oxygen waste through its rapid removal via the high levels of reduced ferrous iron, Fe(II), in the early ocean. He suggested that the oxygen released by photosynthesis oxidized the Fe(II) to ferric iron, Fe(III), which precipitated out of the sea water to form banded iron formation.[62][63] He interpreted the great peak in deposition of banded iron formation at the end of the Archean as the signature for the evolution of mechanisms for living with oxygen. This ended self-poisoning and produced a population explosion in the cyanobacteria that rapidly oxygenated the ocean and ended banded iron formation deposition.[62][63] However, improved dating of Precambrian strata showed that the late Archean peak of deposition was spread out over tens of millions of years, rather than taking place in a very short interval of time following the evolution of oxygen-coping mechanisms. This made Cloud's hypothesis untenable.[19]

Most modern interpretations describe the GOE as a long, protracted process that took place over hundreds of millions of years rather than a single abrupt event, with the quantity of atmospheric oxygen fluctuating in relation to the capacity of oxygen sinks and the productivity of oxygenic photosynthesisers over the course of the GOE.[3] More recently, families of bacteria have been discovered that closely resemble cyanobacteria but show no indication of ever having possessed photosynthetic capability. These may be descended from the earliest ancestors of cyanobacteria, which only later acquired photosynthetic ability by lateral gene transfer. Based on molecular clock data, the evolution of oxygen-producing photosynthesis may have occurred much later than previously thought, at around 2.5 Ga. This reduces the gap between the evolution of oxygen photosynthesis and the appearance of significant atmospheric oxygen.[64]

Nutrient famines

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Another possibility is that early cyanobacteria were starved for vital nutrients, and this checked their growth. However, a lack of the scarcest nutrients, iron, nitrogen, and phosphorus, could have slowed but not prevented a cyanobacteria population explosion and rapid oxygenation. The explanation for the delay in the oxygenation of the atmosphere following the evolution of oxygen-producing photosynthesis likely lies in the presence of various oxygen sinks on the young Earth.[15]

Nickel famine

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Early chemosynthetic organisms likely produced methane, an important trap for molecular oxygen, since methane readily oxidizes to carbon dioxide (CO2) and water in the presence of UV radiation. Modern methanogens require nickel as an enzyme cofactor. As the Earth's crust cooled and the supply of volcanic nickel dwindled, oxygen-producing algae began to outperform methane producers, and the oxygen percentage of the atmosphere steadily increased.[65] From 2.7 to 2.4 Ga the rate of deposition of nickel declined steadily from a level 400 times that of today.[66] This nickel famine was somewhat buffered by an uptick in sulfide weathering at the start of the GOE that brought some nickel to the oceans, without which methanogenic organisms would have declined in abundance more precipitously, plunging Earth into even more severe and long-lasting icehouse conditions than those seen during the Huronian glaciation.[67]

Large igneous provinces

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Another hypothesis posits that a number of large igneous provinces (LIPs) were emplaced during the GOE and fertilised the oceans with limiting nutrients, facilitating and sustaining cyanobacterial blooms.[68]

Increasing flux

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One hypothesis argues that the GOE was the immediate result of photosynthesis, although the majority of scientists suggest that a long-term increase of oxygen is more likely.[69] Several model results show possibilities of long-term increase of carbon burial,[70] but the conclusions are indeterminate.[71]

Decreasing sink

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In contrast to the increasing flux hypothesis, there are several hypotheses that attempt to use decrease of sinks to explain the GOE.[72] One theory suggests increasing lacustrine organic carbon burial as a cause; with more reduced carbon being buried, there was less of it for free oxygen to react with in the atmosphere and oceans, enabling its buildup.[73] A different theory suggests that the composition of the volatiles from volcanic gases was more oxidized.[57] Another theory suggests that the decrease of metamorphic gases and serpentinization is the main key of GOE. Hydrogen and methane released from metamorphic processes are also lost from Earth's atmosphere over time and leave the crust oxidized.[74] Scientists realized that hydrogen would escape into space through a process called methane photolysis, in which methane decomposes under the action of ultraviolet light in the upper atmosphere and releases its hydrogen. The escape of hydrogen from the Earth into space must have oxidized the Earth because the process of hydrogen loss is chemical oxidation.[74] This process of hydrogen escape required the generation of methane by methanogens, so that methanogens actually helped create the conditions necessary for the oxidation of the atmosphere.[41]

Tectonic trigger

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2.1-billion-year-old rock showing banded iron formation

One hypothesis suggests that the oxygen increase had to await tectonically driven changes in the Earth, including the appearance of shelf seas, where reduced organic carbon could reach the sediments and be buried.[75] The burial of reduced carbon as graphite or diamond around subduction zones released molecular oxygen into the atmosphere.[76][77] The appearance of oxidised magmas enriched in sulphur formed around subduction zones confirms changes in tectonic regime played an important role in the oxygenation of Earth's atmosphere.[78]

The newly produced oxygen was first consumed in various chemical reactions in the oceans, primarily with iron. Evidence is found in older rocks that contain massive banded iron formations apparently laid down as this iron and oxygen first combined; most present-day iron ore lies in these deposits. It was assumed oxygen released from cyanobacteria resulted in the chemical reactions that created rust, but it appears the iron formations were caused by anoxygenic phototrophic iron-oxidizing bacteria, which does not require oxygen.[79] Evidence suggests oxygen levels spiked each time smaller land masses collided to form a super-continent. Tectonic pressure thrust up mountain chains, which eroded releasing nutrients into the ocean that fed photosynthetic cyanobacteria.[80]

Bistability

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Another hypothesis posits a model of the atmosphere that exhibits bistability: two steady states of oxygen concentration. The state of stable low oxygen concentration (0.02%) experiences a high rate of methane oxidation. If some event raises oxygen levels beyond a moderate threshold, the formation of an ozone layer shields UV rays and decreases methane oxidation, raising oxygen further to a stable state of 21% or more. The Great Oxygenation Event can then be understood as a transition from the lower to the upper steady states.[81][82]

Increasing photoperiod

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Cyanobacteria tend to consume nearly as much oxygen at night as they produce during the day. However, experiments demonstrate that cyanobacterial mats produce a greater excess of oxygen with longer photoperiods. The rotational period of the Earth was only about six hours shortly after its formation 4.5 Ga but increased to 21 hours by 2.4 Ga in the Paleoproterozoic. The rotational period increased again, starting 700 million years ago, to its present value of 24 hours. The total amount of oxygen produced by the cyanobacteria remained the same with longer days, but the longer the day, the more time oxygen has to diffuse into the water.[83][84][85]

Consequences of oxygenation

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Timeline of glaciations, shown in blue

Eventually, oxygen started to accumulate in the atmosphere, with two major consequences.

  • Oxygen likely oxidized atmospheric methane (a strong greenhouse gas) to carbon dioxide (a weaker one) and water. This weakened the greenhouse effect of the Earth's atmosphere, causing planetary cooling, which has been proposed to have triggered a series of ice ages known as the Huronian glaciation, bracketing an age range of 2.45–2.22 Ga.[86][87][88]
  • The increased oxygen concentrations provided a new opportunity for biological diversification, as well as tremendous changes in the nature of chemical interactions between rocks, sand, clay, and other geological substrates and the Earth's air, oceans, and other surface waters. Despite the natural recycling of organic matter, life had remained energetically limited until the widespread availability of oxygen. The availability of oxygen greatly increased the free energy available to living organisms, with global environmental impacts. For example, mitochondria evolved after the GOE, giving organisms the energy to exploit new, more complex morphologies interacting in increasingly complex ecosystems, although these did not appear until the late Proterozoic and Cambrian.[89]

Mineral diversification

[edit]
Main article: Mineral evolution

The Great Oxygenation Event triggered an explosive growth in the diversity of minerals, with many elements occurring in one or more oxidized forms near the Earth's surface.[90] It is estimated that the GOE was directly responsible for deposition of more than 2,500 of the total of about 4,500 minerals found on Earth today. Most of these new minerals were formed as hydrated and oxidized forms due to dynamic mantle and crust processes.[91]

↓GOE
↓End of Huronian glaciation
Palæoproterozoic
Mesoproterozoic
Neoproterozoic
Palæozoic
Mesozoic
Cenozoic
│
−2500
│
−2300
│
−2100
│
−1900
│
−1700
│
−1500
│
−1300
│
−1100
│
−900
│
−700
│
−500
│
−300
│
−100
Million years ago. Age of Earth = 4,560

Cyanobacteria evolution

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In field studies done in Lake Fryxell, Antarctica, scientists found that mats of oxygen-producing cyanobacteria produced a thin layer, one to two millimeters thick, of oxygenated water in an otherwise anoxic environment, even under thick ice. By inference, these organisms could have adapted to oxygen even before oxygen accumulated in the atmosphere.[92] The evolution of such oxygen-dependent organisms eventually established an equilibrium in the availability of oxygen, which became a major constituent of the atmosphere.[92]

Origin of eukaryotes

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It has been proposed that a local rise in oxygen levels due to cyanobacterial photosynthesis in ancient microenvironments was highly toxic to the surrounding biota and that this selective pressure drove the evolutionary transformation of an archaeal lineage into the first eukaryotes.[93] Oxidative stress involving production of reactive oxygen species (ROS) might have acted in synergy with other environmental stresses (such as ultraviolet radiation and desiccation) to drive selection in an early archaeal lineage towards eukaryosis. This archaeal ancestor may already have had DNA repair mechanisms based on DNA pairing and recombination, and possibly some cell fusion mechanism.[94][95] The detrimental effects of internal ROS (produced by endosymbiont proto-mitochondria) on the archaeal genome could have promoted the evolution of meiotic sex from these humble beginnings.[94] Selective pressure for efficient DNA repair of oxidative DNA damage may have driven the evolution of eukaryotic sex involving such features as cell-cell fusions, cytoskeleton-mediated chromosome movements, and the emergence of the nuclear membrane.[93] Thus, the evolution of eukaryotic sex and eukaryogenesis were likely inseparable processes that largely evolved to facilitate DNA repair.[93] The evolution of mitochondria, which are well suited for oxygenated environments, may have occurred during the GOE.[96]

However, other authors express skepticism that the GOE resulted in widespread eukaryotic diversification due to the lack of robust evidence, concluding that the oxygenation of the oceans and atmosphere does not necessarily lead to increases in ecological and physiological diversity.[97]

Lomagundi-Jatuli event

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The rise in oxygen content was not linear: instead, there was a rise in oxygen content around 2.3 Ga, followed by a drop around 2.1 Ga. This rise in oxygen is called the Lomagundi-Jatuli event, Lomagundi event,[98][99] or Lomagundi-Jatuli excursion[100] (named for a district of Southern Rhodesia) and the time period has been termed Jatulian; it is currently considered to be part of the Rhyacian period.[101][102][103] During the Lomagundi-Jatuli event, oxygen amounts in the atmosphere reached similar heights to modern levels, before returning to low levels during the following stage, which caused the deposition of black shales (rocks that contain large amounts of organic matter that would otherwise have been burned away by oxygen). This drop in oxygen levels is called the Shunga-Francevillian event. Evidence for the event has been found globally in places such as Fennoscandia and the Wyoming Craton.[104][105] Oceans seem to have stayed rich in oxygen for some time even after the event ended.[102][106]

It has been hypothesized that eukaryotes first evolved during the Lomagundi-Jatuli event.[102]

See also

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  • Boring Billion – Earth history between 1.8~0.8 billion years ago, characterized by tectonic stability, climatic stasis, and a slow biological evolution with very low oxygen levels and no evidence of glaciation
  • Neoproterozoic oxygenation event – A second major increase in Earth's oxygen levels that occurred between around 850 and 540 million years ago
  • Geological history of oxygen – Timeline of the development of free oxygen in the Earth's oceans and atmosphere
  • Medea hypothesis – The hypothesis that multicellular life may be self-destructive or suicidal
  • Pasteur point – Switch from fermentation to aerobic respiration
  • Purple Earth hypothesis – Hypothesis that early photosynthesis reflected purple light
  • Rare Earth hypothesis – Hypothesis that complex extraterrestrial life is an extremely rare phenomenon
  • Stromatolite – Layered sedimentary structure formed by the growth of bacteria or algae

References

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  1. ^ Holland, Heinrich D. (19 May 2006). "The oxygenation of the atmosphere and oceans". Philosophical Transactions of the Royal Society: Biological Sciences. 361 (1470): 903–915. doi:10.1098/rstb.2006.1838. PMC 1578726. PMID 16754606.
  2. ^ Margulis, Lynn; Sagan, Dorion (1986). "Chapter 6, "The Oxygen Holocaust"". Microcosmos: Four Billion Years of Microbial Evolution. California: University of California Press. p. 99. ISBN 9780520210646.
  3. ^ a b c Lyons, Timothy W.; Reinhard, Christopher T.; Planavsky, Noah J. (February 2014). "The rise of oxygen in Earth's early ocean and atmosphere". Nature. 506 (7488): 307–315. Bibcode:2014Natur.506..307L. doi:10.1038/nature13068. PMID 24553238. S2CID 4443958.
  4. ^ a b Gumsley, Ashley P.; Chamberlain, Kevin R.; Bleeker, Wouter; Söderlund, Ulf; De Kock, Michiel O.; Larsson, Emilie R.; Bekker, Andrey (6 February 2017). "Timing and tempo of the Great Oxidation Event". Proceedings of the National Academy of Sciences of the United States of America. 114 (8): 1811–1816. Bibcode:2017PNAS..114.1811G. doi:10.1073/pnas.1608824114. ISSN 0027-8424. PMC 5338422. PMID 28167763.
  5. ^ Sosa Torres, Martha E.; Saucedo-Vázquez, Juan P.; Kroneck, Peter M.H. (2015). "The Magic of Dioxygen". In Kroneck, Peter M.H.; Sosa Torres, Martha E. (eds.). Sustaining Life on Planet Earth: Metalloenzymes Mastering Dioxygen and Other Chewy Gases. Metal Ions in Life Sciences volume 15. Vol. 15. Springer. pp. 1–12. doi:10.1007/978-3-319-12415-5_1. ISBN 978-3-319-12414-8. PMID 25707464.
  6. ^ Ossa Ossa, Frantz; Spangenberg, Jorge E.; Bekker, Andrey; König, Stephan; Stüeken, Eva E.; Hofmann, Axel; et al. (15 September 2022). "Moderate levels of oxygenation during the late stage of Earth's Great Oxidation Event". Earth and Planetary Science Letters. 594: 117716. Bibcode:2022E&PSL.59417716O. doi:10.1016/j.epsl.2022.117716. hdl:10481/78482.
  7. ^ Plait, Phil (28 July 2014). "Poisoned Planet". Slate. Retrieved 8 July 2019.
  8. ^ Hodgskiss, Malcolm S. W.; Crockford, Peter W.; Peng, Yongbo; Wing, Boswell A.; Horner, Tristan J. (27 August 2019). "A productivity collapse to end Earth's Great Oxidation". Proceedings of the National Academy of Sciences of the United States of America. 116 (35): 17207–17212. Bibcode:2019PNAS..11617207H. doi:10.1073/pnas.1900325116. ISSN 0027-8424. PMC 6717284. PMID 31405980.
  9. ^ Schirrmeister, Bettina E.; de Vos, Jurriaan M.; Antonelli, Alexandre; Bagheri, Homayoun C. (29 January 2013). "Evolution of multicellularity coincided with increased diversification of cyanobacteria and the Great Oxidation Event". Proceedings of the National Academy of Sciences of the United States of America. 110 (5): 1791–1796. Bibcode:2013PNAS..110.1791S. doi:10.1073/pnas.1209927110. PMC 3562814. PMID 23319632.
  10. ^ Crockford, Peter W.; Kunzmann, Marcus; Bekker, Andrey; Hayles, Justin; Bao, Huiming; Halverson, Galen P.; et al. (20 May 2019). "Claypool continued: Extending the isotopic record of sedimentary sulfate". Chemical Geology. 513: 200–225. Bibcode:2019ChGeo.513..200C. doi:10.1016/j.chemgeo.2019.02.030. ISSN 0009-2541.
  11. ^ Crockford, Peter W.; bar On, Yinon M.; Ward, Luce M.; Milo, Ron; Halevy, Itay (November 2023). "The geologic history of primary productivity". Current Biology. 33 (21): 4741–4750.e5. Bibcode:2023CBio...33E4741C. doi:10.1016/j.cub.2023.09.040. PMID 37827153.
  12. ^ Pavlov, A. A.; Kasting, J. F. (5 July 2004). "Mass-Independent Fractionation of Sulfur Isotopes in Archean Sediments: Strong Evidence for an Anoxic Archean Atmosphere". Astrobiology. 2 (1): 27–41. doi:10.1089/153110702753621321. PMID 12449853. Retrieved 25 September 2022.
  13. ^ Zhang, Shuichang; Wang, Xiaomei; Wang, Huajian; Bjerrum, Christian J.; Hammarlund, Emma U.; Costa, M. Mafalda; et al. (4 January 2016). "Sufficient oxygen for animal respiration 1,400 million years ago". Proceedings of the National Academy of Sciences of the United States of America. 113 (7): 1731–1736. Bibcode:2016PNAS..113.1731Z. doi:10.1073/pnas.1523449113. PMC 4763753. PMID 26729865. Retrieved 13 August 2023.
  14. ^ a b c d e f Kasting, J. (12 February 1993). "Earth's early atmosphere". Science. 259 (5097): 920–926. doi:10.1126/science.11536547. PMID 11536547. S2CID 21134564.
  15. ^ a b c d e Shaw, George H. (August 2008). "Earth's atmosphere – Hadean to early Proterozoic". Geochemistry. 68 (3): 235–264. Bibcode:2008ChEG...68..235S. doi:10.1016/j.chemer.2008.05.001.
  16. ^ Kasting, J. F. (2014). "Modeling the Archean Atmosphere and Climate". Treatise on Geochemistry. Elsevier. pp. 157–175. doi:10.1016/b978-0-08-095975-7.01306-1. ISBN 9780080983004.
  17. ^ a b c d Wiechert, U. H. (20 December 2002). "GEOLOGY: Earth's Early Atmosphere". Science. 298 (5602): 2341–2342. doi:10.1126/science.1079894. PMID 12493902. S2CID 128858098.
  18. ^ Baumgartner, Raphael J.; Van Kranendonk, Martin J.; Wacey, David; Fiorentini, Marco L.; Saunders, Martin; Caruso, Stefano; et al. (1 November 2019). "Nano-porous pyrite and organic matter in 3.5 billion-year-old stromatolites record primordial life" (PDF). Geology. 47 (11): 1039–1043. Bibcode:2019Geo....47.1039B. doi:10.1130/G46365.1. S2CID 204258554.
  19. ^ a b Trendall, A. F. (2002). "The Significance of Iron-Formation in the Precambrian Stratigraphic Record". Precambrian Sedimentary Environments. pp. 33–66. doi:10.1002/9781444304312.ch3. ISBN 978-1-4443-0431-2.
  20. ^ a b Cox, Grant M.; Halverson, Galen P.; Minarik, William G.; Le Heron, Daniel P.; Macdonald, Francis A.; Bellefroid, Eric J.; Strauss, Justin V. (December 2013). "Neoproterozoic iron formation: An evaluation of its temporal, environmental and tectonic significance". Chemical Geology. 362: 232–249. Bibcode:2013ChGeo.362..232C. doi:10.1016/j.chemgeo.2013.08.002. S2CID 56300363.
  21. ^ Large, Ross R.; Hazen, Robert M.; Morrison, Shaunna M.; Gregory, Dan D.; Steadman, Jeffrey A.; Mukherjee, Indrani (May 2022). "Evidence that the GOE was a prolonged event with a peak around 1900 Ma". Geosystems and Geoenvironment. 1 (2): 100036. Bibcode:2022GsGe....100036L. doi:10.1016/j.geogeo.2022.100036.
  22. ^ Warke, Matthew R.; Di Rocco, Tommaso; Zerkle, Aubrey L.; Lepland, Aivo; Prave, Anthony R.; Martin, Adam P.; et al. (16 June 2020). "The Great Oxidation Event preceded a Paleoproterozoic 'snowball Earth'". Proceedings of the National Academy of Sciences of the United States of America. 117 (24): 13314–13320. Bibcode:2020PNAS..11713314W. doi:10.1073/pnas.2003090117. ISSN 0027-8424. PMC 7306805. PMID 32482849.
  23. ^ a b Hodgskiss, Malcolm S. W.; Sperling, Erik A. (20 October 2021). "A prolonged, two-step oxygenation of Earth's early atmosphere: Support from confidence intervals". Geology. 50 (2): 158–162. doi:10.1130/g49385.1. ISSN 0091-7613. S2CID 244621056.
  24. ^ Poulton, Simon W.; Bekker, Andrey; Cumming, Vivien M.; Zerkle, Aubrey L.; Canfield, Donald E.; Johnston, David T. (April 2021). "A 200-million-year delay in permanent atmospheric oxygenation". Nature. 592 (7853): 232–236. Bibcode:2021Natur.592..232P. doi:10.1038/s41586-021-03393-7. hdl:10023/24041. ISSN 1476-4687. PMID 33782617. S2CID 232419035.
  25. ^ Luo, Genming; Ono, Shuhei; Beukes, Nicolas J.; Wang, David T.; Xie, Shucheng; Summons, Roger E. (6 May 2016). "Rapid oxygenation of Earth's atmosphere 2.33 billion years ago". Science Advances. 2 (5): e1600134. Bibcode:2016SciA....2E0134L. doi:10.1126/sciadv.1600134. ISSN 2375-2548. PMC 4928975. PMID 27386544.
  26. ^ Ostrander, Chadlin M.; Heard, Andy W.; Shu, Yunchao; Bekker, Andrey; Poulton, Simon W.; Olesen, Kasper P.; Nielsen, Sune G. (11 July 2024). "Onset of coupled atmosphere–ocean oxygenation 2.3 billion years ago". Nature. 631 (8020): 335–339. doi:10.1038/s41586-024-07551-5. ISSN 0028-0836. PMID 38867053. Retrieved 18 August 2024.
  27. ^ a b c d e f g h Catling, David C.; Kasting, James F. (2017). Atmospheric Evolution on Inhabited and Lifeless Worlds. Cambridge: Cambridge University Press. doi:10.1017/9781139020558. ISBN 978-1-139-02055-8.[page needed]
  28. ^ Utsunomiya, Satoshi; Murakami, Takashi; Nakada, Masami; Kasama, Takeshi (January 2003). "Iron oxidation state of a 2.45 Byr-old paleosol developed on mafic volcanics". Geochimica et Cosmochimica Acta. 67 (2): 213–221. Bibcode:2003GeCoA..67..213U. doi:10.1016/s0016-7037(02)01083-9.
  29. ^ a b Johnson, Jena E.; Gerpheide, Aya; Lamb, Michael P.; Fischer, Woodward W. (27 February 2014). "O2constraints from Paleoproterozoic detrital pyrite and uraninite". Geological Society of America Bulletin. 126 (5–6): 813–830. Bibcode:2014GSAB..126..813J. doi:10.1130/b30949.1. ISSN 0016-7606.
  30. ^ Hofmann, Axel; Bekker, Andrey; Rouxel, Olivier; Rumble, Doug; Master, Sharad (September 2009). "Multiple sulphur and iron isotope composition of detrital pyrite in Archaean sedimentary rocks: A new tool for provenance analysis". Earth and Planetary Science Letters. 286 (3–4): 436–445. Bibcode:2009E&PSL.286..436H. doi:10.1016/j.epsl.2009.07.008. hdl:1912/3068.
  31. ^ Eriksson, Patrick G.; Cheney, Eric S. (January 1992). "Evidence for the transition to an oxygen-rich atmosphere during the evolution of red beds in the lower proterozoic sequences of southern Africa". Precambrian Research. 54 (2–4): 257–269. Bibcode:1992PreR...54..257E. doi:10.1016/0301-9268(92)90073-w.
  32. ^ Trendall, A.F.; Blockley, J.G. (2004). "Precambrian iron-formation". In Eriksson, P.G.; Altermann, W.; Nelson, D.R.; Mueller, W.U.; Catuneanu, O. (eds.). Evolution of the Hydrosphere and Atmosphere. Developments in Precambrian Geology. Developments in Precambrian Geology. Vol. 12. pp. 359–511. doi:10.1016/S0166-2635(04)80007-0. ISBN 978-0-444-51506-3.
  33. ^ a b Canfield, Donald E.; Poulton, Simon W. (1 April 2011). "Ferruginous Conditions: A Dominant Feature of the Ocean through Earth's History". Elements. 7 (2): 107–112. Bibcode:2011Eleme...7..107P. doi:10.2113/gselements.7.2.107.
  34. ^ Lantink, Margriet L.; Oonk, Paul B. H.; Floor, Geerke H.; Tsikos, Harilaos; Mason, Paul R. D. (February 2018). "Fe isotopes of a 2.4 Ga hematite-rich IF constrain marine redox conditions around the GOE". Precambrian Research. 305: 218–235. Bibcode:2018PreR..305..218L. doi:10.1016/j.precamres.2017.12.025. hdl:1874/362652. Retrieved 29 December 2022.
  35. ^ a b c d Lyons, Timothy W.; Anbar, Ariel D.; Severmann, Silke; Scott, Clint; Gill, Benjamin C. (May 2009). "Tracking Euxinia in the Ancient Ocean: A Multiproxy Perspective and Proterozoic Case Study". Annual Review of Earth and Planetary Sciences. 37 (1): 507–534. Bibcode:2009AREPS..37..507L. doi:10.1146/annurev.earth.36.031207.124233.
  36. ^ Scholz, Florian; Severmann, Silke; McManus, James; Noffke, Anna; Lomnitz, Ulrike; Hensen, Christian (December 2014). "On the isotope composition of reactive iron in marine sediments: Redox shuttle versus early diagenesis". Chemical Geology. 389: 48–59. Bibcode:2014ChGeo.389...48S. doi:10.1016/j.chemgeo.2014.09.009.
  37. ^ Farquhar, J. (4 August 2000). "Atmospheric Influence of Earth's Earliest Sulfur Cycle". Science. 289 (5480): 756–758. Bibcode:2000Sci...289..756F. doi:10.1126/science.289.5480.756. PMID 10926533. S2CID 12287304.
  38. ^ Fakhraee, Mojtaba; Hancisse, Olivier; Canfield, Donald Eugene; Crowe, Sean A.; Katsev, Sergei (22 April 2019). "Proterozoic seawater sulfate scarcity and the evolution of ocean–atmosphere chemistry". Nature Geoscience. 12 (5): 375–380. Bibcode:2019NatGe..12..375F. doi:10.1038/s41561-019-0351-5. S2CID 146026944. Retrieved 20 December 2022.
  39. ^ Frei, R.; Gaucher, C.; Poulton, S.W.; Canfield, D.E. (2009). "Fluctuations in Precambrian atmospheric oxygenation recorded by chromium isotopes". Nature. 461 (7261): 250–253. Bibcode:2009Natur.461..250F. doi:10.1038/nature08266. PMID 19741707. S2CID 4373201.
  40. ^ Lyons, Timothy W.; Reinhard, Christopher T. (September 2009). "Oxygen for heavy-metal fans". Nature. 461 (7261): 179–180. doi:10.1038/461179a. PMID 19741692. S2CID 205049360.
  41. ^ a b Kerr, R. A. (17 June 2005). "Earth Science: The Story of O2". Science. 308 (5729): 1730–1732. doi:10.1126/science.308.5729.1730. PMID 15961643. S2CID 129684672.
  42. ^ Konhauser, Kurt O.; Lalonde, Stefan V.; Planavsky, Noah J.; Pecoits, Ernesto; Lyons, Timothy W.; Mojzsis, Stephen J.; et al. (October 2011). "Aerobic bacterial pyrite oxidation and acid rock drainage during the Great Oxidation Event". Nature. 478 (7369): 369–373. Bibcode:2011Natur.478..369K. doi:10.1038/nature10511. PMID 22012395. S2CID 205226545.
  43. ^ Catling, David C.; Zahnle, Kevin J. (February 2020). "The Archean atmosphere". Science Advances. 6 (9): eaax1420. Bibcode:2020SciA....6.1420C. doi:10.1126/sciadv.aax1420. ISSN 2375-2548. PMC 7043912. PMID 32133393.
  44. ^ a b Schopf, J. William (29 June 2006). "Fossil evidence of Archaean life". Philosophical Transactions of the Royal Society B: Biological Sciences. 361 (1470): 869–885. doi:10.1098/rstb.2006.1834. PMC 1578735. PMID 16754604.
  45. ^ Bosak, Tanja; Knoll, Andrew H.; Petroff, Alexander P. (30 May 2013). "The Meaning of Stromatolites". Annual Review of Earth and Planetary Sciences. 41 (1): 21–44. Bibcode:2013AREPS..41...21B. doi:10.1146/annurev-earth-042711-105327. ISSN 0084-6597.
  46. ^ Brocks, Jochen J.; Logan, Graham A.; Buick, Roger; Summons, Roger E. (13 August 1999). "Archean Molecular Fossils and the Early Rise of Eukaryotes". Science. 285 (5430): 1033–1036. Bibcode:1999Sci...285.1033B. doi:10.1126/science.285.5430.1033. PMID 10446042.
  47. ^ French, Katherine L.; Hallmann, Christian; Hope, Janet M.; Schoon, Petra L.; Zumberge, J. Alex; Hoshino, Yosuke; et al. (27 April 2015). "Reappraisal of hydrocarbon biomarkers in Archean rocks". Proceedings of the National Academy of Sciences of the United States of America. 112 (19): 5915–5920. Bibcode:2015PNAS..112.5915F. doi:10.1073/pnas.1419563112. PMC 4434754. PMID 25918387. Retrieved 13 August 2023.
  48. ^ Fadel, Alexandre; Lepot, Kevin; Busigny, Vincent; Addad, Ahmed; Troadec, David (September 2017). "Iron mineralization and taphonomy of microfossils of the 2.45–2.21 Ga Turee Creek Group, Western Australia". Precambrian Research. 298: 530–551. Bibcode:2017PreR..298..530F. doi:10.1016/j.precamres.2017.07.003. Retrieved 19 May 2024 – via Elsevier Science Direct.
  49. ^ Anbar, Ariel D.; Rouxel, Olivier (May 2007). "Metal Stable Isotopes in Paleoceanography". Annual Review of Earth and Planetary Sciences. 35 (1): 717–746. Bibcode:2007AREPS..35..717A. doi:10.1146/annurev.earth.34.031405.125029. S2CID 130960654.
  50. ^ Stüeken, E.E.; Buick, R.; Bekker, A.; Catling, D.; Foriel, J.; Guy, B.M.; et al. (1 August 2015). "The evolution of the global selenium cycle: Secular trends in Se isotopes and abundances". Geochimica et Cosmochimica Acta. 162: 109–125. Bibcode:2015GeCoA.162..109S. doi:10.1016/j.gca.2015.04.033.
  51. ^ Cardona, T.; Murray, J. W.; Rutherford, A. W. (May 2015). "Origin and Evolution of Water Oxidation before the Last Common Ancestor of the Cyanobacteria". Molecular Biology and Evolution. 32 (5): 1310–1328. doi:10.1093/molbev/msv024. PMC 4408414. PMID 25657330.
  52. ^ Tomitani, Akiko (April 2006). "The evolutionary diversification of cyanobacteria: Molecular–phylogenetic and paleontological perspectives". PNAS. 103 (14): 5442–5447. Bibcode:2006PNAS..103.5442T. doi:10.1073/pnas.0600999103. PMC 1459374. PMID 16569695.
  53. ^ "Cyanobacteria: Fossil record". Ucmp.berkeley.edu. Retrieved 26 August 2010.
  54. ^ Dutkiewicz, A.; Volk, H.; George, S.C.; Ridley, J.; Buick, R. (2006). "Biomarkers from Huronian oil-bearing fluid inclusions: An uncontaminated record of life before the Great Oxidation Event". Geology. 34 (6): 437. Bibcode:2006Geo....34..437D. doi:10.1130/G22360.1.
  55. ^ Caredona, Tanai (6 March 2018). "Early Archean origin of heterodimeric Photosystem I". Heliyon. 4 (3): e00548. Bibcode:2018Heliy...400548C. doi:10.1016/j.heliyon.2018.e00548. PMC 5857716. PMID 29560463.
  56. ^ Howard, Victoria (7 March 2018). "Photosynthesis originated a billion years earlier than we thought, study shows". Astrobiology Magazine. Archived from the original on 1 October 2020. Retrieved 23 March 2018.{{cite news}}: CS1 maint: unfit URL (link)
  57. ^ a b Holland, Heinrich D. (November 2002). "Volcanic gases, black smokers, and the great oxidation event". Geochimica et Cosmochimica Acta. 66 (21): 3811–3826. Bibcode:2002GeCoA..66.3811H. doi:10.1016/s0016-7037(02)00950-x.
  58. ^ a b University of Zurich (17 January 2013). "Great Oxidation Event: More oxygen through multicellularity". ScienceDaily.
  59. ^ Anbar, A.; Duan, Y.; Lyons, T.; Arnold, G.; Kendall, B.; Creaser, R.; et al. (2007). "A whiff of oxygen before the great oxidation event?". Science. 317 (5846): 1903–1906. Bibcode:2007Sci...317.1903A. doi:10.1126/science.1140325. PMID 17901330. S2CID 25260892.
  60. ^ Dahl, T.W.; Hammarlund, E.U.; Anbar, A.D.; Bond, D.P.G.; Gill, B.C.; Gordon, G.W.; et al. (30 September 2010). "Devonian rise in atmospheric oxygen correlated to the radiations of terrestrial plants and large predatory fish". Proceedings of the National Academy of Sciences. 107 (42): 17911–17915. Bibcode:2010PNAS..10717911D. doi:10.1073/pnas.1011287107. PMC 2964239. PMID 20884852.
  61. ^ Catling, David C.; Claire, Mark W. (August 2005). "How Earth's atmosphere evolved to an oxic state: A status report". Earth and Planetary Science Letters. 237 (1–2): 1–20. Bibcode:2005E&PSL.237....1C. doi:10.1016/j.epsl.2005.06.013.
  62. ^ a b Cloud, Preston E. (1968). "Atmospheric and Hydrospheric Evolution on the Primitive Earth". Science. 160 (3829): 729–736. Bibcode:1968Sci...160..729C. doi:10.1126/science.160.3829.729. JSTOR 1724303. PMID 5646415.
  63. ^ a b Cloud, P. (1973). "Paleoecological Significance of the Banded Iron-Formation". Economic Geology. 68 (7): 1135–1143. Bibcode:1973EcGeo..68.1135C. doi:10.2113/gsecongeo.68.7.1135.
  64. ^ Blankenship, Robert E. (31 March 2017). "How Cyanobacteria went green". Science. 355 (6332): 1372–1373. Bibcode:2017Sci...355.1372B. doi:10.1126/science.aam9365. PMID 28360281. S2CID 37177062.
  65. ^ "Breathing Easy Thanks to the Great Oxidation Event". Scientific American. Retrieved 6 April 2016.
  66. ^ Konhauser, Kurt O.; Pecoits, Ernesto; Lalonde, Stefan V.; Papineau, Dominic; Nisbet, Euan G.; Barley, Mark E.; et al. (April 2009). "Oceanic nickel depletion and a methanogen famine before the Great Oxidation Event". Nature. 458 (7239): 750–753. Bibcode:2009Natur.458..750K. doi:10.1038/nature07858. PMID 19360085. S2CID 205216259.
  67. ^ Wang, Shui-Jiong; Rudnick, Roberta L.; Gaschnig, Richard M.; Wang, Hao; Wasylenki, Laura E. (4 March 2019). "Methanogenesis sustained by sulfide weathering during the Great Oxidation Event". Nature Geoscience. 12 (4): 296–300. Bibcode:2019NatGe..12..296W. doi:10.1038/s41561-019-0320-z. S2CID 134715298. Retrieved 11 November 2022.
  68. ^ Peng, Peng; Liu, Xu; Feng, Lianjun; Zhou, Xiqiang; Kuang, Hongwei; Liu, Yongqing; Kang, Jianli; Wang, Xinping; Wang, Chong; Dai, Ke; Wang, Huichu; Li, Jianrong; Miao, Peisen; Guo, Jinghui; Zhai, Mingguo (March 2023). "Rhyacian intermittent large igneous provinces sustained Great Oxidation Event: Evidence from North China craton". Earth-Science Reviews. 238: 104352. Bibcode:2023ESRv..23804352P. doi:10.1016/j.earscirev.2023.104352. Retrieved 19 May 2024 – via Elsevier Science Direct.
  69. ^ Kirschvink, Joseph L.; Kopp, Robert E. (27 August 2008). "Palaeoproterozoic ice houses and the evolution of oxygen-mediating enzymes: the case for a late origin of photosystem II". Philosophical Transactions of the Royal Society B: Biological Sciences. 363 (1504): 2755–2765. doi:10.1098/rstb.2008.0024. PMC 2606766. PMID 18487128.
  70. ^ des Marais, David J.; Strauss, Harald; Summons, Roger E.; Hayes, J.M. (October 1992). "Carbon isotope evidence for the stepwise oxidation of the Proterozoic environment". Nature. 359 (6396): 605–609. Bibcode:1992Natur.359..605M. doi:10.1038/359605a0. PMID 11536507. S2CID 4334787.
  71. ^ Krissansen-Totton, J.; Buick, R.; Catling, D.C. (1 April 2015). "A statistical analysis of the carbon isotope record from the Archean to Phanerozoic and implications for the rise of oxygen". American Journal of Science. 315 (4): 275–316. Bibcode:2015AmJS..315..275K. doi:10.2475/04.2015.01. S2CID 73687062.
  72. ^ Luo, Genming; Zhu, Xiangkun; Wang, Shuijiong; Zhang, Shihong; Jiao, Chaoqun (22 June 2022). "Mechanisms and climatic-ecological effects of the Great Oxidation Event in the early Proterozoic". Science China Earth Sciences. 65 (9): 1646–1672. Bibcode:2022ScChD..65.1646L. doi:10.1007/s11430-021-9934-y. S2CID 250065550. Retrieved 12 November 2022.
  73. ^ Spinks, Samuel C.; Parnell, John; Bowden, Stephen A.; Taylor, Ross A.D.; Maclean, Màiri E. (December 2014). "Enhanced organic carbon burial in large Proterozoic lakes: Implications for atmospheric oxygenation". Precambrian Research. 255: 202–215. doi:10.1016/j.precamres.2014.09.026. Retrieved 18 August 2024 – via Elsevier Science Direct.
  74. ^ a b Catling, D.C. (3 August 2001). "Biogenic Methane, Hydrogen Escape, and the Irreversible Oxidation of Early Earth". Science. 293 (5531): 839–843. Bibcode:2001Sci...293..839C. doi:10.1126/science.1061976. PMID 11486082. S2CID 37386726.
  75. ^ Lenton, T.M.; Schellnhuber, H.J.; Szathmáry, E. (2004). "Climbing the co-evolution ladder". Nature. 431 (7011): 913. Bibcode:2004Natur.431..913L. doi:10.1038/431913a. PMID 15496901. S2CID 27619682.
  76. ^ Duncan, Megan S.; Dasgupta, Rajdeep (25 April 2017). "Rise of Earth's atmospheric oxygen controlled by efficient subduction of organic carbon". Nature Geoscience. 10 (1): 387–392. Bibcode:2017NatGe..10..387D. doi:10.1038/ngeo2939. Retrieved 2 May 2023.
  77. ^ Eguchi, James; Seales, Johnny; Dasgupta, Rajdeep (2019). "Great Oxidation and Lomagundi events linked by deep cycling and enhanced degassing of carbon". Nature Geoscience. 13 (1): 71–76. Bibcode:2020NatGe..13...71E. doi:10.1038/s41561-019-0492-6. PMC 6894402. PMID 31807138.
  78. ^ Meng, Xuyang; Simon, Adam C.; Kleinsasser, Jackie M.; Mole, David R.; Kontak, Daniel J.; Jugo, Peter J.; et al. (28 November 2022). "Formation of oxidized sulfur-rich magmas in Neoarchaean subduction zones". Nature Geoscience. 15 (1): 1064–1070. Bibcode:2022NatGe..15.1064M. doi:10.1038/s41561-022-01071-5. S2CID 254175442. Retrieved 2 May 2023.
  79. ^ Köhler, Inga; Konhauser, Kurt O.; Papineau, Dominic; Bekker, Andrey; Kappler, Andreas (June 2013). "Biological carbon precursor to diagenetic siderite with spherical structures in iron formations". Nature Communications. 4 (1): 1741. Bibcode:2013NatCo...4.1741K. doi:10.1038/ncomms2770. PMID 23612282.
  80. ^ American, Scientific. "Abundant Oxygen Indirectly Due to Tectonics". Scientific American. Archived from the original on 28 August 2018. Retrieved 6 April 2016.
  81. ^ Goldblatt, C.; Lenton, T.M.; Watson, A.J. (2006). "Bistability of atmospheric oxygen and the Great Oxidation". Nature. 443 (7112): 683–686. Bibcode:2006Natur.443..683G. doi:10.1038/nature05169. PMID 17036001. S2CID 4425486.
  82. ^ Claire, M.W.; Catling, D.C.; Zahnle, K.J. (December 2006). "Biogeochemical modelling of the rise in atmospheric oxygen". Geobiology. 4 (4): 239–269. Bibcode:2006Gbio....4..239C. doi:10.1111/j.1472-4669.2006.00084.x. S2CID 11575334.
  83. ^ Klatt, J.M.; Chennu, A.; Arbic, B.K.; Biddanda, B.A.; Dick, G.J. (2 August 2021). "Possible link between Earth's rotation rate and oxygenation". Nature Geoscience. 14 (8): 564–570. Bibcode:2021NatGe..14..564K. doi:10.1038/s41561-021-00784-3. S2CID 236780731.
  84. ^ Pennisi, Elizabeth (2 August 2021). "'Totally new' idea suggests longer days on early Earth set stage for complex life". Science. doi:10.1126/science.abl7415. S2CID 242885564.
  85. ^ "Longer days likely bosted Earth's early oxygen". eos.org. 3 September 2021.
  86. ^ Bekker, Andrey (2014). "Huronian glaciation". In Amils, Ricardo; Gargaud, Muriel; Cernicharo Quintanilla, José; Cleaves, Henderson James (eds.). Encyclopedia of Astrobiology. Springer Berlin Heidelberg. pp. 1–8. doi:10.1007/978-3-642-27833-4_742-4. ISBN 978-3-642-27833-4.
  87. ^ Kopp, Robert E.; Kirschvink, Joseph L.; Hilburn, Isaac A.; Nash, Cody Z. (2005). "The Paleoproterozoic snowball Earth: A climate disaster triggered by the evolution of oxygenic photosynthesis". Proceedings of the National Academy of Sciences of the United States of America. 102 (32): 11131–11136. Bibcode:2005PNAS..10211131K. doi:10.1073/pnas.0504878102. PMC 1183582. PMID 16061801.
  88. ^ Lane, Nick (5 February 2010). "First breath: Earth's billion-year struggle for oxygen". New Scientist. No. 2746.
  89. ^ Sperling, Erik; Frieder, Christina; Raman, Akkur; Girguis, Peter; Levin, Lisa; Knoll, Andrew (August 2013). "Oxygen, ecology, and the Cambrian radiation of animals". Proceedings of the National Academy of Sciences of the United States of America. 110 (33): 13446–13451. Bibcode:2013PNAS..11013446S. doi:10.1073/pnas.1312778110. PMC 3746845. PMID 23898193.
  90. ^ Sverjensky, Dimitri A.; Lee, Namhey (1 February 2010). "The Great Oxidation Event and Mineral Diversification". Elements. 6 (1): 31–36. Bibcode:2010Eleme...6...31S. doi:10.2113/gselements.6.1.31.
  91. ^ "Evolution of Minerals". Scientific American. March 2010.
  92. ^ a b
  93. ^ a b c Gross, J.; Bhattacharya, D. (August 2010). "Uniting sex and eukaryote origins in an emerging oxygenic world". Biology Direct. 5: 53. doi:10.1186/1745-6150-5-53. PMC 2933680. PMID 20731852.
  94. ^ a b Hörandl E, Speijer D (February 2018). "How oxygen gave rise to eukaryotic sex". Proceedings of the Royal Society B. 285 (1872): 20172706. doi:10.1098/rspb.2017.2706. PMC 5829205. PMID 29436502.
  95. ^ Bernstein, Harris; Bernstein, Carol (2017). "Sexual communication in Archaea, the precursor to eukaryotic meiosis". Biocommunication of Archaea. pp. 103–117. doi:10.1007/978-3-319-65536-9_7. ISBN 978-3-319-65535-2.
  96. ^ Mänd, Kaarel; Planavsky, Noah J.; Porter, Susannah M.; Robbins, Leslie J.; Wang, Changle; Kreitsmann, Timmu; et al. (15 April 2022). "Chromium evidence for protracted oxygenation during the Paleoproterozoic". Earth and Planetary Science Letters. 584: 117501. Bibcode:2022E&PSL.58417501M. doi:10.1016/j.epsl.2022.117501. hdl:10037/24808. Retrieved 17 September 2023.
  97. ^ Fakhraee, Mojtaba; Tarhan, Lidya G.; Reinhard, Christopher T.; Crowe, Sean A.; Lyons, Timothy W.; Planavsky, Noah J. (May 2023). "Earth's surface oxygenation and the rise of eukaryotic life: Relationships to the Lomagundi positive carbon isotope excursion revisited". Earth-Science Reviews. 240: 104398. Bibcode:2023ESRv..24004398F. doi:10.1016/j.earscirev.2023.104398.
  98. ^ Schidlowski, Manfred; Eichmann, Rudolf; Junge, Christian (1975). "Precambrian sedimentary carbonates: carbon and oxygen isotope geochemistry and implications for the terrestrial oxygen budget". Precambrian Research. 2 (1): 1–69. Bibcode:1975PreR....2....1S. doi:10.1016/0301-9268(75)90018-2.
  99. ^ Schidlowski, Manfred; Eichmann, Rudolf; Junge, Christian (1976). "Carbon isotope geochemistry of the Precambrian Lomagundi carbonate province, Rhodesia". Geochimica et Cosmochimica Acta. 40 (4): 449–455. Bibcode:1976GeCoA..40..449S. doi:10.1016/0016-7037(76)90010-7.
  100. ^ "Research". Earth Evolution Research Group, Department of Geoscience, University of Wisconsin-Madison, USA. Retrieved 29 November 2024.
  101. ^ Strassert, Jürgen F. H.; Irisarri, Iker; Williams, Tom A.; Burki, Fabien (2021). "A molecular timescale for eukaryote evolution with implications for the origin of red algal-derived plastids". Nature. 12 (1): 1879. Bibcode:2021NatCo..12.1879S. doi:10.1038/s41467-021-22044-z. PMC 7994803. PMID 33767194.
  102. ^ a b c Mänd, Kaarel; Lalonde, Stefan V.; Robbins, Leslie J.; Thoby, Marie; Paiste, Kärt; Kreitsmann, Timmu; et al. (April 2020). "Palaeoproterozoic oxygenated oceans following the Lomagundi–Jatuli Event". Nature Geoscience. 13 (4): 302–306. Bibcode:2020NatGe..13..302M. doi:10.1038/s41561-020-0558-5. hdl:10037/19269. S2CID 212732729.
  103. ^ Van Kranendonk, Martin J. (2012). "16: A chronostratigraphic division of the Precambrian: Possibilities and challenges". In Gradstein, Felix M.; Ogg, James G.; Schmitz, Mark D.; Ogg, Gabi M. (eds.). The geologic time scale 2012 (1st ed.). Amsterdam: Elsevier. pp. 359–365. doi:10.1016/B978-0-444-59425-9.00016-0. ISBN 978-0-44-459425-9.
  104. ^ Martin, Adam P.; Condon, Daniel J.; Prave, Anthony R.; Lepland, Aivo (December 2013). "A review of temporal constraints for the Palaeoproterozoic large, positive carbonate carbon isotope excursion (the Lomagundi–Jatuli Event)". Earth-Science Reviews. 127: 242–261. Bibcode:2013ESRv..127..242M. doi:10.1016/j.earscirev.2013.10.006. Retrieved 12 December 2022.
  105. ^ Tang, Hao-Shu; Chen, Yan-Jing; Santosh, M.; Zhong, Hong; Wu, Guang; Lai, Yong (28 January 2013). "C–O isotope geochemistry of the Dashiqiao magnesite belt, North China Craton: Implications for the Great Oxidation Event and ore genesis". Geological Journal. 48 (5): 467–483. Bibcode:2013GeolJ..48..467T. doi:10.1002/gj.2486. S2CID 140672677. Retrieved 12 December 2022.
  106. ^ Kreitsmann, T.; Lepland, A.; Bau, M.; Prave, A.; Paiste, K.; Mänd, K.; et al. (September 2020). "Oxygenated conditions in the aftermath of the Lomagundi-Jatuli event: The carbon isotope and rare earth element signatures of the Paleoproterozoic Zaonega formation, Russia". Precambrian Research. 347: 105855. Bibcode:2020PreR..34705855K. doi:10.1016/j.precamres.2020.105855. hdl:10023/23503. S2CID 225636859.
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