A Hydrogen-Rich Early Earth Atmosphere

See allHide authors and affiliations

Science  13 May 2005:
Vol. 308, Issue 5724, pp. 1014-1017
DOI: 10.1126/science.1106983


We show that the escape of hydrogen from early Earth's atmosphere likely occurred at rates slower by two orders of magnitude than previously thought. The balance between slow hydrogen escape and volcanic outgassing could have maintained a hydrogen mixing ratio of more than 30%. The production of prebiotic organic compounds in such an atmosphere would have been more efficient than either exogenous delivery or synthesis in hydrothermal systems. The organic soup in the oceans and ponds on early Earth would have been a more favorable place for the origin of life than previously thought.

It is generally believed that the existence of prebiotic organic compounds on early Earth was a necessary step toward the origin of life. Biologically important molecules can be formed efficiently in a highly reducing atmosphere (CH4- and/or NH3-rich) (1, 2). They can also be produced efficiently in a weakly reducing atmosphere (3-5), where one important factor influencing the efficiency of production is the ratio of hydrogen to carbon (6-8). However, our current understanding of the composition of early Earth's atmosphere suggests it was neither strongly reducing nor hydrogen-rich. The concentrations of CH4 and NH3 are thought to have been low (9), and the hydrogen mixing ratio is believed to be of the order of 10-3 or smaller (10). Because it is difficult to produce organics in the atmosphere, two directions of research into the origin of life on Earth have become dominant: synthesis of organic compounds in hydrothermal systems, and exogenous delivery of organic compounds to early Earth (11). Here we reexamine the theory of diffusion-limited escape of hydrogen and show that hydrogen escape from early Earth's atmosphere was not as rapid as previously assumed. Hydrodynamic escape should be the dominant mechanism of escape, implying a hydrogen-rich early Earth atmosphere in which organic molecules could be produced efficiently.

The assumption that the escape of hydrogen is limited by diffusion into the heterosphere from below is applicable only when the escape is efficient. For Jeans escape to be efficient, the exobase temperature must be high. This condition is satisfied in the current Earth's atmosphere, where exobase temperatures exceed 1000 K as a result of the efficient absorption of solar ultraviolet (UV) radiation by atomic oxygen. The prebiotic Earth's atmosphere was anoxic and probably contained substantial amounts of CO2 (12), similar to modern Venus or Mars. CO2 absorbs UV, but unlike oxygen, it can effectively radiate energy back to space and keep the exobase temperatures low. The CO2-rich venusian and martian exobases have temperatures of 275 K and 350 K, respectively (13). In the anoxic early Earth's atmosphere with low exobase temperature (14), Jeans escape of hydrogen would have been inhibited. For present-day Earth and Mars atmospheres, which have low hydrogen concentrations, the relatively low hydrogen escape rates caused by nonthermal processes are comparable to the Jeans escape rate (15, 16). It is important to consider how the nonthermal escape rate might increase in an atmosphere with large hydrogen abundance. For an H2O-rich early venusian atmosphere, the maximum limit of the nonthermal hydrogen escape rate (caused by the saturation of ionization of hydrogen atoms, which occurs when the homopause hydrogen mixing ratio reaches 2 × 10-3) is ∼1010 cm-2 s-1 (17). The maximum nonthermal escape rate on early Earth should be similar to that on Venus (18). Given the low Jeans and nonthermal escape rates, the total hydrogen escape rate would not have been in balance with the volcanic H2 outgassing rate on early Earth (10) at the previously suggested hydrogen mixing ratio of 10-3. Instead, hydrogen would have been one of the major constituents in the ancient atmosphere.

H2 can absorb extreme ultraviolet (EUV), as can O2 and CO2, but cannot effectively radiate energy back to space. However, H2 can escape because of its low molecular weight and thereby carry energy away to space in a hydrodynamic hydrogen escape flow. When hydrogen is the major gas in the heterosphere and the major absorber of EUV, the escape of hydrogen would not be diffusion-limited but would be controlled by the solar EUV flux available to drive the escape flow (energy-limited), which would produce an escape rate smaller than the diffusion-limited escape rate.

In this report, we describe the application of a hydrodynamic escape model, which was recently developed to study transonic hydrogen hydrodynamic escape (14), to a hydrogen-rich early Earth's atmosphere. Because the solar EUV radiation level could have been much stronger during the Archean era than today (19), EUV radiation levels ×1, ×2.5, and ×5 that of today were used in the simulations for sensitivity studies.

The velocity distributions in the high-energy input cases (×2.5 and ×5) (Fig. 1A) level off and converge near the upper boundary of the model where the sound speed is exceeded (supersonic flow). Transonic points in the higher-energy input cases (×2.5 and ×5) are near 10 Earth radii (14). Near the upper boundary of the model, the flow velocity is comparable to the escape velocity from the planet. Escape velocity is exceeded by the combination of the flow velocity and the thermal velocity at an altitude below the transonic points. In the ×1 EUV level case, the energy absorbed is not adequate to drive supersonic flow, but escape still occurred. Figure 1B shows the temperature profiles in the corresponding cases. Although the peak temperatures are 700 to 800 K in the high-energy input cases, the temperatures at the exobases (marked by crosses) are in the range of 500 to 600 K because of adiabatic cooling associated with the hydrodynamic escape.

Fig. 1.

(A) Flow velocity profiles in hydrodynamic escape of hydrogen under solar EUV levels ×1, ×2.5, and ×5 that of today. r0 is the distance between the lower boundary and the center of Earth. The homopause hydrogen density is 5 × 1012 cm-3, corresponding to a mixing ratio of 50%. The dashed curve represents the escape velocity from Earth. The transonic point is marked approximately by a circle. The dash-dotted curve shows the difference between the escape velocity and the thermal velocity. The exobases are marked by crosses. (B) Temperature profiles in the corresponding cases. Although the peak temperatures are in the range of 700 to 800 K, the temperature at the exobases (marked by crosses) is low (500 to 600 K).

Figure 2 illustrates our calculated escape rates for varying hydrogen homopause mixing ratios. The Jeans escape rates computed for the exobases are more than one order of magnitude smaller than the corresponding hydrodynamic escape rates because of the low exobase temperatures. If the solar EUV radiation level was 2.5 times that of today and the volcanic hydrogen outgassing rate was 5 times that of today (∼9.25 × 1010 hydrogen molecules cm-2 s-1), a hydrogen mixing ratio of more than 30% could have been maintained everywhere below the homopause by balancing the volcanic hydrogen outgassing with the hydrodynamic escape of hydrogen (Fig. 2). By increasing the solar EUV radiation level to 5 times that of today, the hydrogen mixing ratio could still have been maintained at ∼10%. These mixing ratios are two orders of magnitude greater than the 10-3 hydrogen concentration, considering the diffusion-limited hydrogen escape rate. A hydrogen-rich early Earth's atmosphere could be maintained even for the modest hydrogen outgassing rates appropriate if the oxidation state of Earth's mantle 3.9 billion years ago were the same as it is today.

Fig. 2.

Calculated hydrogen escape rate from early Earth's atmosphere as a function of the homopause hydrogen mixing ratio. The homopause air composition is assumed to be the same as that of today, except for the higher hydrogen concentration and lack of oxygen. The diffusion-limited escape rates, previously assumed to apply, are one or two orders of magnitude greater than the hydrodynamic escape rates because of overestimated exobase temperature. The dotted curve shows the Jeans escape rate as a function of homopause hydrogen mixing ratio under the ×2.5 energy input level for the exobase temperatures that are likely to have been present for early Earth. The lower horizontal line represents the volcanic outgassing rate of hydrogen from the interior of Earth today (∼1.8 × 1010 hydrogen molecules cm-2 s-1) (29). The upper horizontal line is the estimated outgassing rate of hydrogen from the interior of early Earth (∼5 times the outgassing rate today) (30).

The hydrodynamic escape rate increases nearly linearly as the solar EUV radiation level increases (Fig. 3), which reflects the energy-limited nature of the hydrodynamic escape. The slope depends on the hydrogen density at the homopause (20).

Fig. 3.

The hydrogen escape rate increases nearly linearly as the solar EUV level increases. The slope is regulated by the homopause hydrogen density n0.

An early Earth's atmosphere with high hydrogen concentration has important consequences for the origin and evolution of life. Endogenous sources of prebiotic organics, such as production by lightning or photochemistry, are dominant in a reducing early Earth's atmosphere, whereas exogenous sources, such as delivery from space or production in hydrothermal systems, become major contributors in an atmosphere of an intermediate oxidation state (1). To provide more specific examples of the influence of high hydrogen concentration, we consider two organic molecule formation mechanisms, realizing that these are not the only prebiotic organic molecule formation mechanisms that are affected by the high hydrogen concentration.

Both H2 and CO2 are uniformly mixed below the homopause (21, 22), where we have shown that the hydrogen mixing ratio could have been greater than 30%. Most photochemistry of interest occurs well below the homopause. Because the CO2 concentration is likely to be less than 30%, H2/C ratios in early Earth's atmosphere could have been greater than 1 throughout the chemically interesting part of the atmosphere. The formation of certain prebiotic organic compounds in an atmosphere of CO2 or CO by electric discharge is almost as productive as that in an atmosphere of CH4, when H2/C ≥ 1 (7, 8). The conservative estimate of amino acid production rate by electric discharge is 107 kg/year when H2/C ≥ 1 (23). Although early Earth's atmosphere might have been dominated by CO2 immediately after the heavy bombardment period, as continents formed on early Earth, the atmospheric CO2 concentration would decline because of weathering, and the H2/C ratio would become suitable for efficient formation of prebiotic organic compounds through electric discharge. Formation of prebiotic organic compounds by electric discharge at this conservative rate in a hydrogen-rich early Earth's atmosphere would have created an ocean with a steady-state amino acid concentration ∼10-6 mol/liter (24), which is orders of magnitude greater than the amino acid concentration estimated for a hydrogen-poor early Earth's atmosphere (25). This amino acid concentration is highly uncertain because neither the production rate nor the destruction rate is well known. In addition, organic films may have formed at the ocean surface, leading to higher concentrations of organic compounds than in the bulk sea water (26).

Because the magnitude of energy deposition from electric discharge in the ancient atmosphere is poorly understood, it is difficult to predict the exact production rate of organic materials from these sources. Alternatively, organics can be formed through photolysis of methane by Lyman-α (Ly-α) photons with subsequent polymerization. The rate of photochemical haze production is critically dependent on the CH4/CO2 ratio (27). A similar dependence on the CH4/CO2 ratio has been found for hydrogen cyanide (HCN) formation in an atmosphere with N2, CO2, and CH4 (5). We used a one-dimensional photochemical model to study the organic production rate in a hydrogen-rich early Earth's atmosphere (14). Figure 4 shows that the production rate of hydrocarbons is enhanced by about three orders of magnitude (from <107 kg/year to 1010 kg/year) when the hydrogen concentration in early Earth's atmosphere changes from 10-3 to 30%. Hence, the atmospheric production rate of organics through UV photolysis would have been orders of magnitude greater than the rate of either the synthesis of organic compounds in hydrothermal systems or the exogenous delivery of organic compounds to early Earth (28).

Fig. 4.

Hydrocarbon production rate increases rapidly as the hydrogen concentration increases, and exceeds the delivery of organics by interplanetary dust particles (IDPs) for H2 mixing ratios above 10%. pCO2 is the partial pressure of CO2 and fCH4 is the mixing ratio of CH4.

On the basis of our new model of hydrodynamic hydrogen escape, we conclude that diffusion-limited escape theory does not apply to a hydrogen-rich early Earth atmosphere. Rather, the escape of hydrogen was energy limited. Hydrogen mixing ratios greater than 30% could have been maintained in the atmosphere of prebiotic Earth without either invoking huge volcanic hydrogen outgassing rates or assuming a reduced mantle. The efficient production of organics in a hydrogen-rich early Earth's atmosphere would have led to an organic soup in the oceans and ponds on the early Earth. The world ocean could have been the birthplace of life (14).

Supporting Online Material

Materials and Methods

SOM Text


References and Notes

View Abstract

Navigate This Article