Oxidized micrometeorites suggest either high pCO2 or low pN2 during the Neoarchean
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Edited by Thure E. Cerling, University of Utah, Salt Lake City, UT, and approved November 20, 2019 (received for review June 22, 2019)

Significance
Paleosols (ancient soils) have been used to estimate CO2 concentrations during the Archean Eon, 4.0 to 2.5 Ga. However, different paleosol studies disagree with each other and with climate model estimates for ancient CO2 levels. Oxidized iron micrometeorites dated at 2.7 Ga represent a new CO2 proxy with which to compare. These meteorites suggest that CO2 constituted 25 to 50% of the atmosphere at that time. This is easiest to explain if the N2 partial pressure was lower than today so that the atmospheric greenhouse effect was modest and the climate was cool, consistent with evidence for contemporaneous glaciation.
Abstract
Tomkins et al. [A. G. Tomkins et al., Nature 533, 235–238 (2016)] suggested that iron oxides contained in 2.7-Ga iron micrometeorites can be used to determine the concentration of O2 in the Archean upper atmosphere. Specifically, they argued that the presence of magnetite in these objects implies that O2 must have been near present-day levels (∼21%) within the altitude range where the micrometeorites were melted during entry. Here, we reevaluate their data using a 1D photochemical model. We find that atomic oxygen, O, is the most abundant strong oxidant in the upper atmosphere, rather than O2. But data from shock tube experiments suggest that CO2 itself may also serve as the oxidant, in which case micrometeorite oxidation really constrains the CO2/N2 ratio, not the total oxidant abundance. For an atmosphere containing 0.8 bar of N2, like today, the lower limit on the CO2 mixing ratio is ∼0.23. This would produce a mean surface temperature of ∼300 K at 2.7 Ga, which may be too high, given evidence for glaciation at roughly this time. If pN2 was half the present value, and warming by other greenhouse gases like methane was not a major factor, the mean surface temperature would drop to ∼291 K, consistent with glaciation. This suggests that surface pressure in the Neoarchean may need to have been lower—closer to 0.6 bar—for CO2 to have oxidized the micrometeorites. Ultimately, iron micrometeorites may be an indicator for ancient atmospheric CO2 and surface pressure; and could help resolve discrepancies between climate models and existing CO2 proxies such as paleosols.
Earth’s atmospheric O2 concentration is widely believed to have been low prior to ∼2.5 Ga, based on a variety of geologic evidence (1), including multiple sulfur isotopes (2⇓–4). These constraints are relevant to the lower atmosphere but do not necessarily apply to the upper atmosphere. Tomkins et al. (5) proposed that ancient spherical micrometeorites could be used to determine past oxygen concentrations in the upper atmosphere. They extracted 59 iron-type micrometeorites from Pilbara limestone, dated at ∼2.72 Ga, and used the iron oxides contained within them to estimate the amount of O2 the micrometeorites would have encountered as they were melted during entry. These type I cosmic spheres were small Fe-Ni metal meteoroids that totally melted to form spheres during hypervelocity entry into the atmosphere. Their oxygen content was obtained in the mesopause during a brief period of frictional melting. Tomkins et al. (5) concluded that upper atmospheric O2 concentrations must have been close to the modern value, 21% by volume, to create the largely oxidized composition of the micrometeorites. To explain the discrepancy with inferred low O2 concentrations at the surface, they suggested that vertical atmospheric mixing in the Neoarchean could have been inhibited by the presence of a stratospheric organic haze, which would have caused a temperature inversion by absorbing incoming sunlight.
In more detail, Tomkins et al. (5) argued that the micrometeorites would have passed through the upper atmosphere, accelerated by Earth’s gravitational field, and reached maximum temperature and velocity between 85 and 90 km above the surface (6). They posited that melting and quench cooling of these sand grain-size meteorites would have occurred within approximately 2 s between 75 and 90 km, so this is where oxidation should have occurred. Tomkins et al. (5) argued that the micrometeorites must have been oxidized when passing through the atmosphere and not by later alteration, based on the presence of a layer of encasing wüstite (FeO) in some of the micrometeorites, along with the preservation of delicate surface textures. They developed a mathematical model to determine the amount of O2 that would need to have been encountered during atmospheric entry to produce the iron oxides found in the micrometeorites. This included an equilibrium chemical model coupled to a numerical model of meteorite ablation. Tomkins et al. (5) argued that CO2 would have been an ineffective oxidant on its own because of its supposedly sluggish rate of reaction, and therefore free O2 would have been needed to oxidize the meteorites.
These micrometeorite data have recently been reanalyzed by Rimmer et al. (7), who concluded that they require low atmospheric surface pressure (∼0.3 bar) at 2.7 Ga. According to their analysis, this allows H2O to penetrate into the upper atmosphere, where it produces O2 from photodissociation. Zahnle and Buick (8) suggested this previously as a possible oxidation route, although they noted that it would require a much less effective tropopause cold trap than exists today. This solution would require that H2O was a major upper atmospheric constituent in the Rimmer et al. (7) model; however, this does not seem to be the case, based on their figure 2. Instead, the O2 in their atmosphere must be coming from photolysis of CO2, as that is the only species that contains enough O atoms to produce it. (See our analysis below regarding conservation of O atoms with altitude.) Our own model also includes photolysis of CO2, but this process is slower than in the Rimmer et al. (7) model, for reasons that remain to be determined. That said, while we think there may be problems with the Rimmer et al. (7) model, or at least with their interpretations, we do agree that lower atmospheric pressure can help explain the Tomkins et al. (5) data, as it would allow for a higher ratio of CO2:N2. This is a key factor in the analysis presented here.
To test both these theories of micrometeorite oxidation, we used our own 1D photochemical model to create a suite of Archean atmosphere profiles with varying concentrations of atmospheric CO2. Rather than focus exclusively on upper atmospheric O2, as Tomkins et al. (5) did, we included O in our calculations as well, to assess the availability of all forms of oxygen. Furthermore, we reevaluated the efficacy of CO2 as an oxidant and considered atmosphere–particle interactions to determine likely conditions for micrometeorite oxidation in the upper Archean atmosphere. We then simulated the effect of possible CO2 concentrations on surface temperature and pressure, for different values of pN2, using a 1D radiative–convective climate model.
Micrometeorite Oxidation
Entry Physics.
Particles with a diameter of less than 1 mm are too small to generate a bow shock during atmospheric entry (6), meaning that micrometeorites smaller than this do not create the shock waves or gas caps that typically form around larger particles under these conditions. The interaction between the smaller micrometeorites and the atmosphere is therefore thought to be simple, as no shock-induced chemical alteration occurs to the surrounding air during entry. Instead, the micrometeorite is simply slowed by, and may react with, the gas it encounters. Deceleration is a function of momentum exchange, and frictional heating during deceleration is what causes the micrometeorite to briefly melt and quench crystallize. The speed of the micrometeorite decreases by a factor of 1/e for each particle mass column of gas that the micrometeorite impacts, assuming all of the gas momentum is transferred to the micrometeorite. A micrometeorite’s speed would decrease to 0.37 and 0.135 of the initial speed after colliding with gas equal to 1 and 2 particle masses, respectively. Faster micrometeorites would encounter more air while molten because of their greater momentum.
The temperature of an entering micrometeorite depends on its velocity and on the ambient gas density, such that
Depending on size and particle speed, most micrometeorites should contact 1 to 2 equivalent masses of air in the time that they are traveling fast enough to be heated to their melting points. A complication is that the micrometeorites are potentially evaporating some fraction of their mass during entry, and this is strongly dependent on entry angle and initial micrometeorite size. Evaporative mass loss during entry would likely decrease the number of Fe atoms that would need to be reacting with oxidants for the micrometeorite to be fully oxidized. But newly acquired oxygen may be lost as well, and so the uncertainties associated with mass loss make it difficult to constrain in our calculations without knowing more about entry angle and initial size. For this study, we assume that the micrometeorite retains most or all of the oxygen it encounters, along with its own initial mass, so oxidizing the micrometeorites is therefore a function of how much oxygen the meteorite encounters in the upper atmosphere while molten.
Tomkins et al. (5) assumed that the altitude region within which the micrometeorites were molten would be the same in the Archean as it is in the modern atmosphere (between ∼75 and 90 km, as ref. 6 specified). But the deceleration—and frictional heating—of a micrometeorite depends on the number of particles it encounters during entry. Thus, the window in which oxidation occurs is not located at a fixed altitude range, but rather at a fixed pressure range. Pressure in our model Archean atmosphere falls off more rapidly than in the modern atmosphere (SI Appendix, Fig. S1B) because of the cooler, ozone-poor stratosphere, along with the higher mean molecular weight caused by increased CO2. Thus, the “oxidation altitude range” of 75 to 90 km for the modern atmosphere should really be redefined as an “oxidation pressure range” from ∼2.3 × 10−5 bar to ∼1.6 × 10−7 bar. The corresponding altitude of oxidation therefore varies with the CO2 concentration and is generally lower than assumed by Tomkins et al. (5) (Table 1).
Approximate altitude of lower and upper bounds of oxidation pressure range for atmospheres with various CO2 mixing ratios
Micrometeorite Oxidation Chemistry.
In a Neoarchean atmosphere with a primarily N2-CO2 composition, upper atmospheric chemistry would be dominated by the reaction
Tomkins et al. (5) considered O2 only as a potential oxidant, assuming that the concentration of other forms of oxygen would be negligible. Their figure 4 shows calculations by Zahnle et al. (9) that appear to support this assumption. But our own photochemical model of the 2.7-Ga atmosphere indicates that both O2 and O would be present in the stratosphere (Photochemical Calculations). The Zahnle et al. model (9, 10), which is a derivative of our model, would almost certainly yield the same result. However, those authors were focused on the lower atmosphere and simply did not include O in their figure.
It is also possible—even likely—that CO2 itself was an oxidant for the micrometeorites. Tomkins et al. (5) argued that Fe oxidation by CO2 would be slow, based on studies of Fe metallurgy at temperatures below 1,470 K (11, 12). But iron micrometeorites (and iron oxide) need to reach at least ∼1,770 K during entry to melt (6). Shock tube experiments above the Fe melting temperature indicate that oxidation rates of Fe to FeO by O2 (13) and CO2 (14) are roughly equal and are up to 3 orders of magnitude faster than reduction of FeO by CO (15). Other possible oxidation reactions include O2 oxidation of Fe to FeO2 (16) and CO2 oxidation of FeO to FeCO3 (17) at similar reaction rates. But it is worth noting that O can also reduce FeO to form O2 in the upper mesosphere (18), albeit at much lower temperatures than the micrometeorites would experience during entry. Until experimental chemical reaction rate data are obtained for the appropriate temperature and pressure range, we cannot definitively state which oxidation and reduction reactions are likely to dominate. Nonetheless, the CO2 oxidation pathway indicates the value such experiments would have for micrometeorite analysis—and, for now, existing data point to its potential significance for the Tomkins micrometeorites. In short, it suggests that at least one O atom from each CO2 molecule may contribute to micrometeorite oxidation during entry. It also suggests that reduction of the newly formed Fe oxides by CO is unlikely to occur during the short time that the micrometeorite is molten and that accumulating an adequate amount of oxidant in the oxidation pressure range is more important than the ratio of oxidants to reductants.
If so, then one should consider the oxidation potential from O, O2, and CO2 within the oxidation pressure window. And this, in turn, makes the calculation quite simple, as nearly all O and O2 in the upper atmosphere is derived from CO2. O atoms are neither created nor destroyed in the atmosphere above the altitude at which they are removed by rainout of H2O. Thus, from mass balance, it is easy to demonstrate (SI Appendix) that if O2 concentrations are low near the surface, and if H2O concentrations are low at the tropopause, then
To make this analysis more concrete, consider the modern atmosphere, within which we know that incoming metal micrometeorites are partly to fully oxidized to form a mix of Fe(1-x)O (wüstite), Fe3O4, and sometimes iron metal during entry (6). For total oxidation, this requires the addition of 1 to 1.3 O atoms per iron atom. In the modern atmosphere, this oxidation is accomplished almost exclusively by O2. Assume for now that the particle remains molten, and hence reactive, only during its encounter with the first equivalent air mass. Because the atomic mass of Fe (∼56 amu) is just under twice the average atmospheric mass (29.6 for N2-O2-40Ar), the micrometeorite should encounter about twice as many air molecules as it contains Fe atoms while it is still molten. Of these, 21% are O2 molecules. Therefore, the ratio of O2 molecules encountered to Fe atoms within the micrometeorite is equal to 2 × 0.21 ≅ 0.4. The ratio of O:Fe is twice that, or 0.8. This ratio is close enough to the O:Fe ratio required to form the observed oxides (as the micrometeorites contain some varying fraction of Ni instead of Fe), provided that oxidation is total and nearly 100% efficient. We can express this relationship compactly by writing
Vertical profiles of major constituents mixing ratios for fCO2 = 25%, close to our minimum estimated value. The pressure range for micrometeorite oxidation is indicated by the shaded yellow region. The modern O2 mixing ratio is shown by the vertical dotted line. Atmosphere also contains 0.8 bar N2.
Suppose now that the meteorite remains molten during its encounter with 2 equivalent air masses. The required CO2 mixing ratio is lower, but not exactly by a factor of 2. The analog to Eq. 7 is
Similar calculations can be performed for the case when CO2 is not considered to be an oxidant for Fe. We do this here because it remains unclear which assumption is actually correct. In this case, CO2 and N2 would still be the dominant constituents in the oxidation pressure range, so Mat remains unchanged, but the fraction of oxidant is fOoxy ≡ (fO + 2 fO2), rather than fCO2. Thus, if the particle remains molten during encounter with one equivalent air mass, we can write
Photochemical Calculations
Methods.
Photochemical model calculations are required if CO2 is not included as a possible oxidant for Fe micrometeorites. For our calculations, we used a version of our 1D photochemical model developed for high-CO2, low-O2 atmospheres (19). Our model contains 49 chemical species involved in 221 reactions (see supporting information in ref. 20 for the full list). It extends upward from the Earth’s surface to 100 km in 1-km thick layers. Vertical mixing is parameterized as a combination of eddy and molecular diffusion, using a profile appropriate for the modern atmosphere (21). Absorption and scattering of solar radiation were calculated using a 2-stream algorithm (22), assuming a fixed solar zenith angle of 50°. The time-dependent, coupled chemistry/diffusion equations were integrated to steady state using the (fully implicit) reverse Euler method. We also calculated changes to the solar UV flux using a parameterization developed by Ribas et al. (23). Properly scaling the UV flux is essential for this analysis, as the rate of free oxygen production via CO2 photolysis depends on this parameter. At 2.7 Ga, the Sun would have been only ∼81% as bright as today in the visible wavelength range (24, 25), but ∼50% brighter than today at far-UV wavelengths (<1,750 Å).
Calculations were performed for a 1-bar, CO2-N2 atmosphere with 1 to 50% CO2, along with low concentrations of methane (below). We should note that we are solving minor-constituent diffusion equations for major species, which introduces some error in the ratio of CO2:CO:O at high altitudes in the model atmosphere. However, this should have little effect on our results because, as discussed earlier, it is only the sum of CO2, O2, and O that matters, as iron reduction by CO is slow. Furthermore, the largest errors in these ratios occur close to the top of the model atmosphere, above the altitude range at which most meteorite oxidation occurs.
We assumed a simplified temperature structure that decreases from 285 K at the surface to 175 K at 9.5 km and then remains constant above that height (SI Appendix, Fig. S1A). This is consistent with predictions from 1D climate models (e.g., ref. 26), which suggest that the temperature profile of an ozone-free atmosphere should follow a moist adiabat from the surface up to the tropopause and then become roughly isothermal above that altitude. We have not attempted to keep the surface temperature consistent with the assumed CO2 concentration and solar flux in these calculations, reasoning that upper atmospheric composition should be relatively insensitive to this parameter. We examine the implications of atmospheric composition and photochemistry on surface temperature in our climate calculations (Discussion).
An upward CH4 flux of 3.0 × 109 molecules⋅cm−2⋅s−1 was assumed for our photochemical calculations. This is about 3% of the present CH4 flux and well below the estimated CH4 flux during the Archean (27). Unlike Tomkins et al. (5), we do not rely on a stratospheric temperature inversion to help build up upper atmospheric O2, and so we avoid the regime in which fCH4/fCO2 > 0.1 and in which organic haze may form (28). The actual amount of CH4 present should have little effect on micrometeorite oxidation; however, it does have implications for climate at that time, so we return to this issue in Discussion.
Data for both photochemical and climate model calculations are available on request from the corresponding author.
Results.
Vertical profiles of major atmospheric constituents for our 25% CO2 case are shown in Fig. 1. Key reducing and oxidizing species in the upper atmosphere at different CO2 concentrations are shown in SI Appendix, Fig. S2. Both O and O2 are present within the micrometeorite oxidation pressure range, with O dominating in the upper part of this region and O2 in the lower part. In all these simulations, the sum of fO + 2fO2 (fOoxy) is much less than fCO2. That is because virtually all of the O and O2 is coming from CO2 and because CO2 itself is relatively resistant to photolysis (CO2 photolyzes only below ∼200 nm, where the solar UV flux is relatively low). Accumulating large amounts of O and O2 in the stratosphere would require unrealistically low eddy mixing. Tomkins et al. (5) argued that such low mixing might result from a stratospheric temperature inversion caused by the presence of organic haze. But the eddy diffusion profile used here already accounts for this phenomenon, as it was derived for the modern stratosphere which has a temperature inversion caused by ozone.
Even with CO2 concentrations as high as 50%, the fraction of the atmosphere within the oxidation pressure range that is composed of O and O2 combined is less than 2% (SI Appendix, Fig. S2). Oxidizing the micrometeorites with oxygen alone (Eq. 9) requires reaching a value of fOoxy roughly 10 times higher than this. Doing so would thus require both an extremely high CO2 concentration and extremely low eddy mixing. It is therefore difficult, or even impossible, to oxidize the Tomkins et al. (5) micrometeorites using just O and O2, unless O2 was abundant throughout the atmosphere. But this possibility is ruled out by geologic data, including sulfur isotope studies, as mentioned earlier. It is much more likely that the micrometeorites were oxidized by CO2, in which case the limits on fCO2 derived in Micrometeorite Oxidation Chemistry remain applicable.
Discussion
Constraints on pCO2 from Neoarchean Climate.
The high atmospheric CO2 concentrations required to oxidize the micrometeorites can be compared with CO2 levels required to explain the climate of the Neoarchean Earth. Ojakangas et al. (29) have reported diamictites dated at 2.7 Ga in the Dharwar Supergroup, India. This is approximately the same age as the micrometeorites (2.721 ± 0.004 Ga) analyzed by Tomkins et al. (5). Even more convincing evidence for glaciation is found in 2.9-Ga rocks from the Pongola Supergroup in South Africa (30). Together, these observations suggest that the climate of the Neoarchean was not too different from that of today. In a long-term sense, Earth’s climate is glacial today because ice caps exist at both poles.
Approximate constraints on global mean surface temperature, TS, during glacial periods have been estimated by Kasting (31), and we follow the same approach here. The modern value of TS is ∼288 K. Polar ice caps were absent during the early Cenozoic and preceding Mesozoic eras. The Antarctic ice cap started to grow about 35 My ago, at which time TS was about 5 °C warmer than today, or 293 K, based on oxygen isotopes in deep sea carbonate cores. This suggests that 293 K is a reasonable upper limit for continental-scale glaciation. The argument is not ironclad, because changes in land–sea distributions—in particular, the opening of the Drake passage at about this same time—could also have helped trigger Antarctic glaciation. But we use this as a reasonable guess at the upper limit on TS at 2.7 Ga. At the same time, we can take 0 °C, or 273 K, as a reasonable lower limit on TS, as climate models predict that Earth’s climate would go into a Snowball state if temperatures were to drop much below this value. Climate theory (32) then predicts that silicate weathering would slow, and atmospheric CO2 would build up if this were the case.
We used an existing 1D climate model (33) to study the effects of high atmospheric CO2 levels on Neoarchean climate. To do so, we needed to first establish a relationship between fCO2 (the CO2 mixing ratio) and surface pressure. This relationship is nonlinear because the total atmospheric pressure changes as fCO2 increases, given a fixed amount of N2. The required relationship (derived in SI Appendix) is
Results from our 1D climate model. (A) Surface temperature as a function of fCO2, for atmospheres with 0.8 bar (purple) and 0.4 bar (green) of N2. Solid curves are for zero CH4; dashed curves are for 1,000 ppm CH4. Blue shaded region denotes subfreezing global mean surface temperatures; orange shaded region indicates a global mean surface temperature too high to facilitate glaciation (main text). The 1- and 2-air-mass oxidation lines represent the fCO2 needed for oxidation to occur if the micrometeorite reacts with these amounts of air during entry. (B) Surface pressure versus fCO2 for a N2-CO2 atmosphere with 0.8 bar N2 (purple) and 0.4 bar N2 (green), as calculated from Eq. 11 in the main text.
The results show that if
The results are more promising for a potentially glacial climate if
All of this suggests that if the micrometeorite oxidation story—with CO2 facilitating Fe micrometeorite oxidation by up to 2 air masses during entry—is correct, levels of pN2 must have been appreciably lower than those today back at 2.7 Ga. While some theoreticians have argued just the opposite (34), more recent authors have provided empirical support for this hypothesis. For example, analysis of vesicles in 2.7-Ga basaltic lavas erupted at sea level imply PS < 0.5 bar (35), and measured N2/36Ar ratios in fluid inclusions trapped in 3- to 3.5-Ga hydrothermal quartz suggest PS < 1.1 bar to possibly as low as 0.5 bar (36, 37). All 3 of these estimates are consistent with the low pN2 and PS values derived here.
Constraints on pCO2 from Paleosols.
Archean CO2 levels have also been estimated from paleosols. Driese et al. (38) published an estimate of 10 to 50 PAL (times the Present Atmospheric Level) CO2 at ∼2.7 Ga, based on an analytical technique developed by Sheldon (39). A total of 1 PAL CO2 corresponds to 370 ppmv, or 3.7 × 10−4 bar, in their model, so their estimate is ∼0.004 to 0.02 bar. By comparison, our minimum estimates of pCO2 are ∼0.16 bar for the 0.4-bar pN2 case and ∼0.25 bar for the 0.8-bar pN2 case (these are true CO2 partial pressures—hence, no prime on pCO2—obtained by multiplying fCO2 = 0.23 by the corresponding surface pressure in SI Appendix, Fig. S1B). Our pCO2 estimates are clearly much higher than Sheldon’s (39) estimates. But Sheldon’s method of analysis can be criticized on several different grounds (40). Most importantly, it implicitly assumes that every CO2 molecule that enters the soil will react with a silicate mineral, which is probably not the case. Hence, his method should provide only a lower limit on atmospheric pCO2. A more recent analysis of the same paleosols by Kanzaki and Murakami (41) yields pCO2 values ranging from 0.03 bar to almost 0.4 bar (Fig. 3). The upper end of these estimates overlaps nicely with the CO2 partial pressures derived here. So, ∼0.2 bar might be considered a “best guess” of atmospheric pCO2 at the time when the Tomkins et al. (5) micrometeorites fell to Earth. At the very least, the pCO2 estimates from micrometeorite oxidation provide support for the higher Kanzaki and Murakami (41) pCO2 estimates from paleosols compared to the older estimates from Driese et al. (38) and Sheldon (39).
pCO2 estimates from paleosols compared to those from climate model calculations (gray shaded region) (31). Estimates from Sheldon (39) are shown by the black squares and solid black line (with error in yellow). The dashed vertical bar is the paleosol estimate at 2.7 Ga from Driese et al. (38). The downward red arrow is the upper pCO2 limit from cyanobacterial sheath calcification at 1.2 Ga (Kah and Riding, ref. 42). The vertical bars in blue are the paleosol estimates from Kanzaki and Murakami (41). The upward pink arrow indicates the pCO2 from our calculations at 2.7 Ga if pN2 was 0.8 bar. Reproduced from ref. 43 with permission of Cambridge University Press through PLSclear.
Conclusions
To truly solve this problem, experimental data on iron oxidation by CO2, O, and O2 in conditions like those a micrometeorite would experience during entry are needed. Nonetheless, existing data support the idea that the oxidation of Archean iron micrometeorites, melted during atmospheric entry, depends primarily on the amount of CO2 available in the atmosphere. Assuming 2-air-mass oxidation and that CO2 itself is the primary oxidant, we find that at least ∼23% CO2 would be needed to oxidize the Tomkins et al. (5) micrometeorites at 2.7 Ga. This CO2 concentration can be reconciled with values derived from paleosols, provided that one accepts the higher estimates of Kanzaki and Murakami (41). It is most easily reconciled with climate models if levels of pN2 were lower than they are today, as this would facilitate a global mean surface temperature low enough for glaciation to occur. A surface pressure of about 0.6 bar, with less than 25% CO2, would have allowed the Tomkins et al. (5) micrometeorites to be oxidized without conflicting with the evidence for glaciation at 2.7 Ga. There is thus no need to invoke unusually high atmospheric O2 concentrations to explain the micrometeorite oxidation. Instead, these oxidized micrometeorites imply a Neoarchean atmosphere that was rich in CO2 and somewhat poorer in N2 than today’s atmosphere.
Acknowledgments
We (R.C.P. and J.F.K.) thank Benjamin P. Hayworth for his contributions to our analysis of the chemical and physical aspects of micrometeorite oxidation.
Footnotes
- ↵1To whom correspondence may be addressed. Email: rebeccapaynercp{at}gmail.com.
Author contributions: R.C.P. and J.F.K. designed research; R.C.P. performed research; R.C.P. contributed new reagents/analytic tools; R.C.P., D.B., and J.F.K. analyzed data; R.C.P. and J.F.K. wrote the paper; and D.B. assisted with conceptual work.
The authors declare no competing interest.
This article is a PNAS Direct Submission.
This article contains supporting information online at https://www.pnas.org/lookup/suppl/doi:10.1073/pnas.1910698117/-/DCSupplemental.
Published under the PNAS license.
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