Probing space to understand Earth


Progress in the geosciences has often followed the same fundamental paradigm for about two centuries: Earth’s present is the key to understanding its past and its future. This concept is at the root of most of what is known about the Earth. Similarly, knowledge of Earth’s geological and atmospheric processes can be, and has been, applied when studying the history of other planetary bodies. More recently, however, observations from other planets have fed back into our understanding of Earth. In this Perspective, we argue that many scientific mysteries about the Earth can be solved only by looking beyond it, and describe instances where other bodies, such as Mars, Venus and the Moon, have or could augment our understanding of processes on Earth. Future space missions offer the opportunity to probe the rich diversity of planetary environments and compositions, and further explore how they might serve as analogues, experiments and archives.


Most of what we know about our planet is derived from observations of its present state and inference about its past through the lens of the physical and life sciences. Assuming that the laws of physics and chemistry as we observe them on Earth are valid across the Universe, mechanistic knowledge of Earth’s geological and atmospheric processes can be applied to understand the past, present and future of other planetary bodies. Although Galileo arguably pioneered this approach by comparing the Moon’s valleys, plains and mountains to those of Earth1, this scientific endeavour has expanded rapidly in the last century2,3,4,5,6,7,8,9,10 (sometimes through trial and error!2).

In turn, knowledge gained from exploring other planetary bodies can inform us about our own planet. In 1980, R. Sharp remarked that “planetary exploration has proved to be a two-way street”11, and in the following 40 years, researchers have applied new lessons from throughout the Solar System to studies of Earth. The study of planetary atmospheres, in particular, has led to numerous advances in understanding Earth’s atmosphere, including how life might have affected it (originated by Lovelock’s classic work on the prospect for life detection on Mars12), the physics of nuclear, volcanic and impact winters (motivated by observations of a global dust storm on Mars13) and a deeper understanding of the greenhouse effect (aided by application of the radiation-transfer equations to other planets14). Since the first confirmed detection of an exoplanet in 1992, exoplanetary science has also provided new insight into the formation of the Solar System and the Earth15,16. However, the approach of utilizing other planetary bodies to learn about our own has not permeated all of the Earth sciences equally, and is only starting to make its way into, for example, the mechanics of sedimentary processes.

In this Perspective, we explore how the multitude and variety of planetary bodies within (Fig. 1) and beyond17,18 (Box 1) our Solar System present new crucial observations that might be key to resolving some fundamental mysteries about the Earth. There are multiple Earth analogues in the Solar System (and more beyond) that could provide insights into Earth’s history and future. Even when planetary bodies are not analogous to Earth, they span a range of sizes, environments and compositions that allow us to approach comparative planetology as a grand, full-scale experiment to systematically develop quantitative models of geological and atmospheric processes that pertain to our understanding of the Earth. Finally, planets, moons and other small bodies might have recorded critical pieces of Earth’s history that were not preserved in Earth’s geological archive. New data from ongoing, upcoming and future planetary missions and telescopic observations of alien worlds are poised to provide new insights into these planetary bodies and, thus, potentially, Earth.

Fig. 1: Venus, Earth, the Moon and Mars through time.

Despite being Earth’s closest neighbours, Venus, the Moon and Mars display a diverse array of surface conditions today (including surface gravity, g; surface temperature, T; atmospheric pressure at the surface, p; and the presence of liquid water) and size (planetary radii, R). Their respective geologic records vary greatly, both in terms of age and magnetic, tectonic and volcanic processes. Displayed here is how a selection of planetary attributes for Venus, Earth, the Moon and Mars evolved through time as inferred from currently available data. Through their similarities and differences, other celestial bodies can be utilized (both in their present state and inferred past) as analogues to ancient, modern and future Earth, as experiments to understand how geological and atmospheric processes operate under conditions that are unachievable on Earth, and as geological archives that hold clues to deciphering Earth’s past. Gya, billion years ago.

Planetary bodies as analogues

The Earth has undergone several major transitions throughout its history, including the formation of its core, the onset of its dynamo, the formation and evolution of an early atmosphere, the initiation of plate tectonics and the advent of life. The exploration of our Solar System has revealed a multitude of planetary environments that provide analogues to Earth at various stages of its multifaceted history. As plate tectonics is continuously erasing parts of Earth’s geologic record, the surface record of Earth’s early history is sparse and highly altered, necessitating a look towards extraterrestrial worlds. In this section, we present four research topics and associated major questions about the Earth that can be addressed by exploiting analogies between early Earth and other planetary bodies.

Core and dynamo formation

Palaeomagnetic records suggest that the Earth’s magnetic field has been continuously active throughout the past 3.5 billion years (Gy) or longer (Fig. 1), with intensities overall comparable to that of the modern-day field throughout most of its history19,20. However, models of Earth’s thermal evolution suggest that the core is cooling by ~100 K/Gy, such that crystallization of the inner core — which drives the chemical convection in the outer core that produces Earth’s magnetic field today — initiated less than 1.5 billion years ago (Gya)21,22. Core nucleation ~1.5 Gya is also suggested by an inferred increase in palaeointensity values around that time20. As a result, our current understanding of the processes that sustain the Earth’s magnetic field is at odds with the palaeomagnetic record. This discrepancy is known as the new core paradox23,24 and raises the question of how Earth’s dynamo could have started so early and still be long-lived. As palaeomagnetic studies of Earth’s Hadean to Palaeoarchaean eons are ambiguous25,26, solving the new core paradox may require that we turn towards other worlds.

Exoplanetary magnetic fields have been identified for Jupiter-sized exoplanets orbiting close to their star, called hot Jupiters27, and it might soon be feasible to detect these fields for smaller, rocky planets. Exoplanetary magnetic fields might, therefore, reveal whether Earth’s long-lived dynamo is statistically anomalous28 and, thus, required special circumstances to form. For example, mechanical mixing of the Earth’s core by the Moon-forming impact could have been needed to remove chemical stratification that would have otherwise precluded a dynamo29, even if the core had a ‘hot start’ (that is, was initially hot relative to the overlying mantle) and was cooling rapidly enough to drive thermal convection in the absence of adverse chemical gradients.

While Mars, the Moon and Venus (Fig. 1) lack strong intrinsic magnetic fields today, they might teach us about the core-formation processes that enabled Earth’s long-lived dynamo and whether those processes are ubiquitous or rare. The well-preserved record of a >4-billion-year-old dynamo on Mars30 (Fig. 1) is reproduced in models that include a hot start to core formation31, which supports the hypothesis that a similarly hot start to Earth’s core could have driven a Hadean dynamo. Like the Earth, the Moon presents a paradox, as purely thermal core convection is likely insufficient to generate magnetic fields as long-lived or as intense as those inferred from the 4.25 Gy lunar palaeomagnetic record32 (Fig. 1).

Chemical convection might have increased the longevity and strength of the lunar dynamo33. Nevertheless, the identification of a long-lived magnetic field on the Moon motivated preliminary research into dynamos driven by mechanical processes such as librations (the wobbling of an orbiting body as perceived from the orbited body), precession (a change in the direction of a body’s axis of rotation) and tides34. All of these processes can kinematically sustain a dynamo in simulations35. However, further work is needed to fully understand the interplay between turbulence, magnetic fields and the Lorentz force (electromagnetic force) within planetary cores to determine whether mechanically driven flows could present a solution to the new core paradox23,36.

Unresolved questions about the lunar dynamo also prompted research into dynamos generated within basal magma oceans37 (layers of molten silicates immediately above the core–mantle boundary), as has been proposed for the early Earth38,39,40,41. For example, core convection in Earth’s Moon may provide insufficient energy to sustain a lunar dynamo for the duration and at the intensities indicated by palaeomagnetic data42. Instead, the Moon’s dynamo could have been generated for much of its lifetime in a basal magma ocean, where high titanium and iron contents could have bolstered its electrical conductivity43 to values three orders of magnitude higher than that of olivine melts at lunar mantle conditions37. If future studies confirm that liquid silicates have high enough electrical conductivity under basal mantle conditions44 and, thus, support this method of dynamo generation, there would be a dramatic shift away from conventional thinking that early dynamos must be generated in planetary cores.

The Moon and Mars are too small to have experienced the extreme pressures and temperatures required for chemical processes, such as the precipitation of magnesium oxide or silicon dioxide45,46,47,48, that might have sustained Earth’s early magnetic field prior to the crystallization of its inner core. These conditions could have occurred within Venus though, which is Earth’s near-twin in size and bulk composition49,50. Unveiling the unknown magnetic history of Venus by searching for crustal remanent magnetism could reveal that Earth and Venus had a very similar early history or that stochastic variability during planetary accretion set them on different evolutionary paths from the start50.

Earth’s atmosphere through time

Earth’s very first atmosphere likely formed through a number of processes, including magma ocean devolatilization51 and impact degassing52. Models for the growth of Earth’s atmosphere thus rely on the composition of the materials present during the time of planet formation, but geological evidence from this era is limited. However, asteroid-derived meteorites that formed at the beginning of the Solar System provide a window into the chemical gradients that existed across the solar nebula during planet formation53. Thus, models for the growth and composition of Earth’s earliest atmosphere can be developed by using meteorites as proxies for the materials that were delivered to the growing planets during the formation of the Solar System. The bulk and isotopic compositions of the different meteorite groups suggest that a large portion of Earth’s volatiles are derived from carbonaceous-chondrite-like material54. Accretion of this material appears to have led to the formation of an early steam atmosphere on the Earth, and plausibly on Venus55.

Water acts as a major greenhouse gas and can cause widespread melting of silicates at the surface. As a result, the lifetime of a magma ocean (which can result from giant impacts) can be extended by several orders of magnitude if a massive steam atmosphere is present56. This greenhouse warming is more effective for planets receiving higher stellar fluxes. Thus, whereas Earth’s magma ocean following the Moon-forming impact might have only lasted 1–5 million years (Myr), a magma ocean could have lasted up to 100 Myr on Venus due to the planet’s closer solar orbit57.

While magma oceans might have only existed in the first ~100 Myr of Solar System history, steam atmospheres and magma oceans from giant impacts could be identifiable in young exoplanetary systems, making it possible to observe some of the fundamental processes that built the Earth into what it is today58. In addition, exoplanetary magma oceans could be long-lived on warm-to-hot rocky exoplanets, owing to greenhouse warming from massive atmospheres (potentially as on 55 Cancri e)59 or extreme solar radiation in the case of plausibly atmosphere-less planets (as on CoRoT-7b and Kepler 10b). Observations of atmospheric signatures from such planets (like the presence of gases composed of silicate material60,61) could help us understand the underlying magma oceans. Observations of the effects of magma oceans or steam atmospheres on exoplanets would provide a unique opportunity to constrain atmosphere–interior-exchange models62 for the early Earth.

Planetary analogues not only speak to Earth’s very first atmosphere but also provide insights into Earth’s later atmospheric evolution. In one example, studies of the greenhouse and anti-greenhouse effects on Titan63 led to multiple insights into the mechanisms (such as organic hazes) that could have helped keep Earth warm and shielded the surface from ultraviolet radiation, despite a faint young Sun (Fig. 2) and lack of ozone layer in the Hadean and early Archaean64,65,66. Additionally, the recent realization that Earth’s atmospheric N2 inventory has varied through time67,68 has inspired modelling of exoplanets with different N2 inventories. This modelling revealed that exoplanets in the so-called habitable zone of their star (Fig. 2) can build up O2-dominated atmospheres due to water photolysis when their N2 levels are low69,70,71. This means that atmospheres with notable O2 contents can form without biological activity, which has implications for the hunt for life around other stars. Along with palaeopressure and composition proxies for Earth’s atmosphere72,73, this realization is leading to new thinking on Earth’s potential rate of oxidation via hydrogen loss in the Archaean74,75 as a function of its N2 inventory through time76,77.

Fig. 2: A shifting ‘habitable zone’ with greenhouse warming and the faint young Sun.

The habitable zone (shaded areas) for a planet with a 1-bar atmosphere, fixed orbital distance around a Sun-like star and fixed albedo (visible reflectivity) shifts when the greenhouse effect is considered (shown here for +0 K, +30 K or +60 K of greenhouse warming). In the absence of atmospheric greenhouse gases (black lines, +0 K), liquid water is predicted to be stable at Venus’ orbital radius, whereas only ice would be thermodynamically stable at Earth’s and Mars’ radii. However, with greenhouse gases, Venus’ equilibrium surface temperature is raised by ~510 K and is uninhabitable, whereas greenhouse gases raise Earth’s equilibrium surface temperature by ~30 K, making Earth habitable. Approximately 4 billion years ago (Gya), the young Sun is thought to have been less bright, so the outer edge of the habitable zone would have been shifted to smaller orbital radii. Explaining the abundance and sustainability of surface flows on Mars 4 Gya requires the addition of significant greenhouse gases to its atmosphere or that the Sun was once more massive (indicated by the dashed horizontal line).

In another example, large volcanic eruptions throughout Earth’s history (both explosive and effusive) emitted dust, ash and sulfate aerosols to the atmosphere, triggering major environmental changes and, potentially, mass extinctions78. Starting as far back as the 1970s79,80, studies of sulfate aerosols on Venus81 and other planets of the Solar System82 have helped increase our understanding of their climate impact on Earth. This has led to new insights into the possible role of sulfate aerosols in past mass extinctions83,84,85 and Snowball-climate transitions86, and, more controversially, their potential for use in intentional solar-radiation management (solar geoengineering) in the future87.

Insights into Earth’s early stellar-radiation history have been provided by observations of nearby Sun-like stars of varying ages, which have helped to constrain the Sun’s bolometric and extreme ultraviolet luminosity evolution88,89. Escape of hydrogen and helium from exoplanetary atmospheres has already been inferred from these observations90,91. Predictions of atmospheric escape from Earth will be improved by future observations of gas escape from Earth-like planets, which will allow us to validate models of escape from Earth’s atmosphere through time. Planetary science is, hence, fundamental to developing a robust understanding of Earth’s atmospheric evolution, and the interplay between the two fields is deepening in the modern exoplanet era.

Initiation of plate tectonics

In the absence of substantial geological materials from Earth’s early days, understanding how (and when) plate tectonics started is complex92,93. A promising approach is to look at Earth’s planetary neighbours, which did not develop plate tectonics but may have undergone a similar geodynamic regime as the early Earth. For example, the absence of plate tectonics on Venus and Mars today might, by comparison, provide clues as to how the Earth developed plate tectonics in the past. Venus, which has a younger surface than Earth on average94 (Fig. 1), could operate in a similar geodynamic regime as an early Earth that featured plume-induced subduction95. Enigmatic Venusian tectonic features such as coronae (Box 2) might provide clues to the initiation of plate tectonics on Earth if they are sites of incipient subduction (as indicated by their morphology and correlations between gravity and topography). Lithospheric conditions for Venus today are similar to those for Archaean Earth, when the mantle was ~200 K hotter and the thermal lithosphere was thinner96. Venusian tesserae (Box 2) have unknown compositions at present but, based on their morphology and surface emissivity97, they might be analogous to granitic continents on Earth. A felsic composition for tesserae would indicate that they formed in the presence of large volumes of water98, which would support the hypothesis that the loss of surface water on Venus is responsible for the limited extent of subduction today, whereas long-lived oceans sustain plate tectonics on Earth93.

Surface processes and geochemical cycles before life

Several planetary bodies of the Solar System display ancient surfaces that predate Earth’s oldest rocks. For example, a significant fraction of the Martian surface is older than 3.5 Gy and, thus, formed during Earth’s Hadean and Archaean eons (more than 2.5 Gya)99. Mars, which experienced significant surface geological activity early in its history (Fig. 1), offers the Solar System’s longest known record of geological, hydrological and, possibly, biological processes100. Sedimentary rocks observed by the National Aeronautics and Space Administration (NASA) Curiosity rover at Gale crater, for instance, offer a unique window into aeolian101, fluvial102 and lacustrine103,104 processes on Mars at a time when microscopic life is believed to have already evolved on Earth105,106, but long before macroscopic organisms colonized the Earth’s surface.

Life profoundly affects the workings of Earth’s surface processes, from rock weathering, soil formation and erosion, to longer-term climate feedbacks that, in turn, control sediment fluxes across Earth’s surface107. For example, river functioning is intricately tied to vegetation on Earth today108. Meandering rivers with muddy floodplains, in particular, are thought to have co-evolved with land plants and to only have become prevalent with the greening of the continents109,110, but the pre-life fluvial record of Earth is relatively poor110. In contrast, the surface of Mars hosts many meandering-river deposits111,112 dating back to the planet’s wet past, offering a unique window into the formation of meandering rivers in the absence of land plants. Understanding Martian river sedimentology will allow us to develop and test new facies models for unvegetated, meandering rivers113 and quantify the rates of associated processes, such as lateral channel migration114. Thus, Martian river deposits might hold the key to interpreting the pre-Silurian rock record of Earth113, which, in turn, has direct implications for the duration of sediment storage within fluvial floodplains and, therefore, the pace of geochemical cycling and Earth’s palaeoclimate114,115.

Biological cycling dominates the distribution and availability of elements both critical and peripheral to life functions on Earth today, even creating new minerals116. In terrestrial conditions, it is extremely difficult to understand the availability of different elements at the time when or before life formed, or to isolate abiotic-element-cycling processes. Samples from small bodies, such as iron meteorites, and Mars could be used to identify and isolate abiotic elemental cycling (such as the Martian phosphorus cycle117) from biological effects. Information about extraterrestrial element cycles can then be used to understand the contribution of abiotic cycling on early Earth and the potential availability of key elements when life first arose118. Earth-sized and super-Earth-sized planets also provide a wealth of analogues for prebiotic Earth volatile cycles in chemical and mass parameter spaces that are not available in our Solar System119 (Box 1). The carbonate–silicate cycle, for instance, is the basis of habitable zone models120, and statistical tests of these models have been proposed121 that would evaluate the validity of geological controls on atmospheric CO2 by comparing measurements of its atmospheric abundance in a large sample of planets with model predictions. Such tests must await the next generation of space telescopes (such as the Large Ultraviolet Optical Infrared Surveyor, or LUVOIR, and the Habitable Exoplanet Observatory, or HabEx), which may be capable of making these measurements for small, cool habitable-zone worlds.

Planetary bodies as experiments

Developing complex geological and atmospheric models requires knowledge or estimation of all possible controlling factors, either through laboratory and field-based experiments or observations. However, it is often not possible to test all controlling factors on Earth and, as a result, the predictive power of our models is often hindered by our inability to account for unknowns. Owing to their diverse physical and chemical characteristics, planetary bodies can serve as full-scale experiments, allowing us to probe parts of parameter spaces that are unachievable on Earth and refine our mechanistic understanding of geological and atmospheric processes (Box 3). Here, we present three research topics with associated major questions regarding the geological and atmospheric processes that can be tackled by utilizing the diversity of the planetary bodies in our Solar System (Figs 1,3) and beyond (Box 1).

Fig. 3: Large wind ripples on Mars: an experiment that challenges our understanding of aeolian ripple formation, and a likely analogue to terrestrial current ripples.

a | Two scales of aeolian ripples (decimetre and metre) atop a basaltic sand dune within the Bagnold dune field of Gale crater, Mars. b | Decimetre-scale aeolian ripples in the Mesquite Flat sand dunes, Death Valley, California, USA. c | Decimetre-scale current ripples on the dry bed of the Amargosa River, Death Valley, California, USA. Part a credited to NASA/JPL-Caltech/MSSS.

Tectonic regimes

Earth, the only planet in the Solar System that clearly exhibits plate tectonics, has abundant water in its crust and upper mantle122. Hydration of Earth’s asthenosphere, in particular, is thought to have played an important role in the onset of plate tectonics123. For example, hydration could lead to weakening and cooling of the lithosphere, which would facilitate convection, lithospheric failure and subduction124. However, this paradigm was questioned recently125. Observations from planets of different sizes, water contents and water distributions (Fig. 1) will, therefore, aid understanding of the precise mechanisms by which water contributes to plate tectonics.

Venus is similar in size to Earth but is water-poor near the surface122,126,127 and shows no evidence of plate tectonics. Mars is, conversely, much smaller than Earth and has (or had) water in its interior and at its surface (Fig. 1), but it too has no known plate tectonics122. It is, thus, possible that larger planets retain higher concentrations of water in their upper mantles (as opposed to being more evenly distributed throughout the entire mantle) as an outcome of magma-ocean solidification and overturn, and that this internal water distribution increases the likelihood that Earth-sized planets develop plate tectonics128. On Earth, plate tectonics is sustained by the subduction of surface water back into the upper mantle, but this process cannot occur on Venus because its crust is dry. It is possible that Earth and Venus had similar initial water contents and internal distributions, but Venus was later dehydrated (perhaps by impacts or hydrodynamic escape that was exacerbated by Venus’ closer proximity to the Sun129,130). The hypothesis that larger rocky planets are more likely to have water in their upper mantles could be tested in the future by measuring the water content of mantle-derived materials from Mars, such as lherzolites and other peridotites. These water contents could be compared with both terrestrial values123 and results from thermal models for planetary interiors that systematically investigate the effect of variable initial water distributions and concentrations.

Some models131 suggest that the current tectonic regime of exoplanets can, in principle, be determined from their surface temperature (calculated after measuring bulk atmospheric properties) and size. Definitive atmospheric (or other) signatures of plate tectonics have not yet been identified. However, the presence of liquid surface water, which is possibly detectable through surface glint132, would be indicative of surface temperatures that support the formation of long-lived discrete plates. Since no other planet is currently known to operate in a plate-tectonic regime, observations that indicate its occurrence on another planet would help to constrain the driving forces behind plate tectonics and potentially inform our understanding of when and how it began on the Earth.

Runaway-greenhouse atmospheres

The presence of a global surface ocean on Earth sets the Blue Marble apart from the other planetary bodies of the Solar System (Fig. 1). Indeed, Earth is the only planet in the Solar System that is able to stably host liquid water at its surface today (Fig. 2). However, it is unknown what will happen to the Earth’s oceans and habitability as thermonuclear fusion continues to brighten the ageing Sun. Venus’ runaway-greenhouse hypothesis14 is a classic example of how another planet can serve as a full-scale experiment for understanding Earth’s possible future. In this scenario, as the young Sun became brighter, a critical luminosity threshold was eventually reached, where Venus’ surface rapidly became hotter and water vapour accumulated in the atmosphere. The resulting greenhouse effect caused a runaway increase in surface temperatures that ultimately evaporated any oceans, and, subsequently, nearly all of Venus’ hydrogen was lost to space14. Although Earth today is still believed to be safe from such a catastrophic transition, Venus’ atmospheric evolution provides a sobering perspective on how much climate can change with only small changes in external forcing.

Observations from Earth-like low-mass planets that are close to their host star (such as GJ1132b62 and the TRAPPIST-1 system133,134) could help to guide our understanding of the runaway-greenhouse phenomenon. A better understanding of the runaway-greenhouse effect, likely through a dialogue between new observations of Venus and exoplanets135, will be key to testing whether Earth’s habitable conditions are common and understanding how our Sun impacts Earth’s habitability. For instance, this research might confirm whether plate tectonics played a critical role in maintaining the long-term habitability of Earth as the Sun brightened120. The carbonate–silicate cycle has provided a pathway through which CO2 could be extracted from the atmosphere and stored in rocks as insolation rose in response to the brightening Sun. If widespread among exoplanets, such feedbacks would effectively stabilize planets against runaway processes related to the evolution of their own stellar hosts136.

Bedforms and sediment transport

Bedforms, such as ripples and dunes, are found throughout the Solar System and are created when a fluid flows over a granular bed, such as water on sand and gravels137, winds on sand138, hydrocarbon flows on water-ice grains139, winds on methane-ice grains140 or even thermal winds on cometary regolith141 (Fig. 3; Box 3). Bedforms represent prime palaeoenvironmental indicators on Earth because they are formed in concert with environmental flows and are preserved in the rock record. However, their use as an indicator requires a quantitative mechanistic understanding of their formation. Our current understanding of bedform-formation processes, which is primarily based on terrestrial observations, can be tested using the extraterrestrial bedforms within our Solar System138,140,141,142,143.

Metre-scale ripples formed by winds in fine sand, for example, appear to be common on Mars but are nowhere to be found on Earth138,144,145 (Fig. 3). Their identification challenges state-of-the-art models, calling for a reappraisal of the underlying ripple-formation mechanics138. Several new models have been proposed to explain the large Martian ripples138,146,147, leading to new insights in the formation of both fluvial147,148 and aeolian138,146,147 bedforms with direct applications to terrestrial environments and their sedimentary record. These applications include the formulation of a new palaeoenvironmental technique to reconstruct flow characteristics from stratigraphy148 and the reappraisal of the conditions required to initiate sand transport.

For example, until recently, it was assumed that a relatively high threshold wind speed149 was required to initiate the saltation (or hopping) of sand grains on Mars. Missions to the Martian surface, though, have revealed that winds rarely exceed that minimum wind speed150,151,152. Nevertheless, active sand transport has been observed globally on Mars from orbiter-based imagery153,154 and locally by rovers155,156,157, challenging our Earth-based understanding of windblown-sand fluxes. To solve this apparent contradiction, new quantitative models that account for the detailed physics of grain-to-grain collisions, grain splash and sporadic saltation clusters have been developed and suggest a greatly decreased (maybe up to about an order of magnitude lower, depending on grain size) threshold wind speed to sustain and even initiate sand transport149,158,159,160. Furthermore, owing to the virtual absence of chemical weathering today, Mars offers an exotic picture of mineral sorting during transport, providing critical insights into how mafic and felsic phases partition along transport pathways due to, for example, crystal size, mineral density and grain shape161,162,163,164,165.

Space as an archive

Between the transformation of the early Earth by the Moon-forming impact, the alteration of Earth’s surface by the hydrosphere and atmosphere, and continuous recycling by tectonics, key pieces of Earth’s history have gone missing from the geologic record. Here, we argue that some of these pieces were not completely lost and can be found by looking towards space. We illustrate how space exploration could help us to reconstruct or infer parts of Earth’s lost archive through three example research topics and associated questions about Earth’s history.

Building Earth

It is likely that the Earth formed in a similar cosmic environment to the thousands of exoplanets known to date (Box 1). Specifically, a gaseous protoplanetary disc would have persisted for 1–10 Myr, followed by a period lasting roughly 100 Myr characterized by giant impacts between planetary embryos within a gas-free environment. Only by observing young analogues of our Sun can important details of these early phases be deduced. For example, young gaseous discs are often permeated with gaps and rings, likely caused by the existence of forming planets166. Together, discoveries of giant planets occupying extremely close-in orbits, planetary chains in orbital resonance (in which orbital periods are close to integer ratios) and gaps in circumstellar discs are strong indicators that planets undergo significant radial migration during the gaseous protoplanetary disc stage. Later, during the gas-free disc stage, the four giant planets in our solar system potentially migrated in their orbits as they gravitationally interacted with solids left over from the planet-building process16. For example, a period of migration (first inwards, then outwards) has been proposed for Jupiter, in which its early path sculpted the inner Solar System and hindered the growth of Mars167. Additionally, young Solar analogues reveal strong magnetic fields and rapid (1–10 days) rotation rates, which expel the disc gas closest to the star during the first 10 Myr and drive a strong Solar wind during the subsequent 100 Myr, a period of time during which the Earth was still forming. The influence of these winds in the early Solar System remains mysterious and could have included an outwards motion of planetary building blocks from the now empty region interior to Mercury’s orbit168 and atmospheric erosion in close-in planetary atmospheres169.

Meteorites have long been used to infer the primordial history of the Solar System and the Earth54,170,171,172,173,174,175,176,177,178. Other examples of possible cosmic archives relevant to Earth’s history come from exoplanetary debris. Spectral observations of these objects (as can be found around white dwarf stars179 or even within our own Solar System180) reveal that exoplanetary rocky materials are, overall, similar in chemical composition to those of Earth181, suggesting that the Earth did not experience a fundamentally different chemical evolution than these objects. Perhaps even more directly, observations of protoplanetary discs will help us answer key questions about the materials that went into forming Earth. For example, Earth is substantially depleted in carbon and nitrogen relative to the interstellar medium (the background material and radiation in a galaxy)182. The only way to understand this depletion is through understanding the chemistry of protoplanetary discs. With the advent of large ground-based telescopes such as the Vera C. Rubin Observatory (previously the Large Synoptic Survey Telescope, or LSST) and the Atacama Large Millimeter/submillimeter Array (ALMA), more observations of exoplanetary debris183 and protoplanetary discs166 might disclose new clues about the building blocks of our planet.

The lunar archive

The Moon is an archive of some of Earth’s early processing, as its highlands have not been significantly modified since the Moon’s formation. For example, lunar samples from the Apollo missions have been used to date Earth’s core formation by comparing the Hf-W isotopic compositions of the Earth and Moon184. Lunar crustal zircons have also constrained the timing of the giant Moon-forming impact to about 4.51 Gya and subsequent lunar magma-ocean crystallization185,186. The magma ocean would have solidified over ~10 Myr, although tidal heating from Earth likely caused the melting and recrystallization of portions of the lunar crust for an additional ~200 Myr187.

In addition, characterizing Earth’s bombardment history188 is critical to understanding the surface environment of Hadean Earth189. Based on lunar rocks, it was proposed that the Moon recorded a spike in cratering approximately 3.9 Gya — a hypothesis that came to be known as the Late Heavy Bombardment190. However, this hypothesized cratering-rate spike has recently been widely challenged, as this interpretation could be the result of sampling biases191. Regardless, because the Moon shares its circumstellar orbit with Earth, it offers a unique record of the impact history at Earth’s orbital radius that is not preserved on Earth itself. Resolving the bombardment history of Earth, therefore, will likely require that we look towards the Moon and other celestial bodies, such as meteorites.

Finally, in addition to its cratering record, the Moon might carry yet another record of Earth’s early days in the form of meteorites that came from Earth. A potential Earth meteorite was recently identified in Apollo 14 samples192. If a terrestrial origin is confirmed, this rock offers a truly unique window into the Hadean and Archaean Earth.

A faint young Sun

It is believed that, about 4 Gya, the young Sun was only 70–75% as bright as today193, leading to an apparent faint young Sun paradox194: under a dimmer Sun, how could liquid water have been stable at the surface of Earth and Mars (Fig. 2)? This problem can be resolved, in principle, if greenhouse gases like CO2, CH4, NH3 or H2 were present in Earth’s early atmosphere64,195,196,197. Nevertheless, the paradox itself rests upon numerous assumptions regarding the early Earth and its geologic record. For example, potential biases could exist in the abiotic deposition of sedimentary records (such as carbonates) that make the early Earth appear warmer than it truly was198. Moreover, the paradox could, in principle, be solved without a substantially enhanced greenhouse effect if the Sun was once more massive199. For the young Sun to have been more massive, the magnitude of the ancient Sun’s winds would have been required to far exceed that of its current winds. Whereas measured mass-loss rates by Sun-like stars confirm that wind magnitudes are generally greater in younger stars, the Sun’s ancient winds would need to be anomalously strong to entirely solve the faint young Sun paradox200.

Avenues to test the massive young Sun hypothesis are few, owing to the inherent difficulty of measuring the Sun’s historical mass. Helioseismology (the study of the Sun’s interior through its oscillations), for example, has been used to investigate the problem but has not been able to confirm or refute a large mass loss201,202. Another way to test this hypothesis would be to constrain the early Solar magnetic field from meteorites203, although extracting a signal from the early Sun is greatly complicated by any remanent magnetism from an intrinsic dynamo of the meteorite’s parent body204.

Despite these difficulties, modelling of the whole Solar System has shown that, throughout solar mass loss, there is a linear relationship between the Sun’s mass and the frequency of orbital oscillations associated with the modern Milankovitch frequency of ~405,000 years205,206. A promising direct test of the massive young Sun hypothesis will be to constrain the variation of the Milankovitch frequencies through time using observations of old, pristine banded sediments. Mars, in particular, is an ideal target to test this idea, as its sedimentary record is longer than Earth’s and it has thick sequences of quasiperiodically layered sediments at its surface that might reflect an astronomical forcing207,208. The feasibility of measuring the signals on Mars will strongly depend upon the chronometers that will be sent to the planet in the future and, perhaps more critically, on the success of sample return to Earth209. Proposed atmospheric compositions thought to be characteristic of the early Earth hinge critically upon Solar insolation197. Thus, testing the massive young Sun hypothesis would help us understand the conditions under which Earth’s earliest life forms emerged.


The dialogue between the Earth and planetary sciences is at the root of many recent advances and discoveries. An important aspect of this dialogue — what space can teach us about our own planet — will likely yield even more exciting results and surprises about the Earth in the future.

Several advances are foreseeable in the short-to-medium term. For example, numerical modelling of mantle evolution within planets could test how different initial conditions (such as water content and distribution) affect a planet’s tectonic regime and can readily provide insights into the initiation of plate tectonics on Earth. Furthermore, detections of exoplanetary magnetic fields via radio, far-ultraviolet auroral or H3+ infrared auroral emissions are now within reach27 and will eventually enable statistical studies of dynamos in terrestrial planets. Observations of exoplanetary magnetic fields could reveal correlations between magnetic field strength or lifetime and planetary attributes such as size, atmospheric mass or rotation rate.

In addition to modelling and statistical studies, telescopic observations could soon provide clues about our planet’s infancy. For instance, under the classic Moon-forming-giant-impact model210, the incredibly close agreement between the oxygen isotopes of the Earth and Moon requires the impactor to have had nearly identical oxygen isotopic composition to the proto-Earth. Although not impossible, the low likelihood of such a scenario has led to the revision of the classic giant-impact hypothesis and to the proposal that the Moon formed in a synestia (a rapidly spinning, non-hydrostatic body of vaporized rock)211. Telescopic observations of giant impacts in other planetary systems, which are technologically achievable today, would confirm that they are a common process and could, by analogy, support the giant-impact hypothesis. The planned James Webb Space Telescope will enable the observation of much older star systems than its predecessors212 and should provide a wealth of new data on planetary formation that can directly augment our understanding of Earth’s birth. The Parker Solar Probe (launched in 2018) could also help us understand Earth in its infancy by measuring solar energetic particles, allowing deeper insight into how they have affected the inner planets213.

Planned space missions will also provide a wealth of new data that will directly feed back into our understanding of the Earth. NASA’s and the European Space Agency’s (ESA) next Mars rovers will investigate ancient surface and subsurface aqueous environments. These rovers should provide new data on geological processes in the absence of macroscopic life that will inform our understanding of Precambrian Earth. The Mars 2020 rover, in particular, will acquire a series of samples to be returned to Earth through a Mars sample-return mission orchestrated by NASA and the ESA. These samples could provide critical constraints on the timing and magnitude of Solar System events that directly impacted Earth’s history, including, possibly, the origins of life118,209. NASA’s Psyche orbiter will launch in 2022 to explore the metal-rich 16 Psyche asteroid, seeking to answer fundamental questions about planetary cores and possibly offering our first direct look at a protoplanetary core fragment. NASA’s Dragonfly mission will send a small rotorcraft to Titan in 2026, which, upon arrival in 2034, will explore what might constitute an atmospheric analogue for the early Earth and offer a glimpse into Earth-like sedimentary processes operating in a world dominated by water ice, nitrogen and hydrocarbons.

Looking further into the future, several fundamental questions could be readily addressed by exploration missions. The NASA-led Artemis programme intends to send a crewed mission to the Moon’s south pole within a decade. The crew will collect lunar rocks from a location that is far from the near-equatorial Apollo landing sites and return them to Earth, where they will undergo a new generation of laboratory analyses that will provide insight into the chemical and physical heterogeneity of the lunar crust and, for example, allow us to test the Late-Heavy-Bombardment hypothesis. Measurements of water content within extraterrestrial materials that contain components derived from upper mantles, which could be collected by lunar and Mars sample-return missions, would provide quantitative constraints to models of plate-tectonics initiation.

Additionally, in situ palaeomagnetic studies and observations of remanent crustal magnetism on the Moon and other planetary bodies by rovers or through low-altitude-flight measurements would inform us on the occurrence and longevity of planetary dynamos and, thus, on how Earth has protected its life forms from dangerous solar winds and cosmic rays for billions of years. Although some crustal palaeomagnetic data exist for the Moon, Mars and Mercury, their coverage and spatial resolution do not permit the timing and duration of their respective dynamos to be inferred. A return to the Moon, such as through the Artemis programme, will enable the collection of oriented samples that will leverage accurate determinations of the ancient lunar magnetic-field structure214.

In contrast to the Moon, Mars and Mercury, no palaeomagnetic data from Venus have been acquired to date. In addition to constraining Venus’ magnetic past and core history, a robotic mission to Venus could determine the extent of its similarity to the early Earth. Compositional measurements of the Venusian surface and atmosphere would help determine whether it ever hosted a surface-water ocean, providing direct clues to Earth’s response to a brightening Sun. More measurements of noble-gas isotopic ratios in the Venusian atmosphere are, in principle, straightforward and would teach us about atmospheric accretion and loss processes215,216. High-resolution geophysical investigations of Venus’ elastic thickness and heat flow would highlight potential differences with the Earth’s lithosphere and inform our understanding of Earth’s geodynamic past.

We will likely never know everything about Earth and its history, but a complete understanding of the Earth system will require that we explore the totality of Earth’s environments, from its core outwards. As one of the last largely unexplored terrestrial environments, the oceans are often referred to as Earth’s final frontier, but this vision relies on the assumption that only Earth can teach us about the Earth. Rather, we argue that Earth’s final frontier is much vaster than its oceans — space could be the key to solving fundamental mysteries about our own planet. Space exploration, however, is a laborious endeavour, and even the most mundane tasks conducted by geoscientists on Earth will likely prove to be complex when performed on another planet. Thus, a continued effort in advancing exploration technology, as well as a robust planetary exploration programme, will be instrumental to gaining further extraterrestrial insights about Earth.


  1. 1.

    Galilei, G. in Sidereus Nuncius (Thomas Baglioni, 1610).

  2. 2.

    Sinton, W. M. Further evidence of vegetation on Mars. Science 130, 1234–1237 (1959).

  3. 3.

    Lowell, P. in Mars (Houghton, Mifflin and Company, 1895).

  4. 4.

    Wallace, A. R. in Is Mars Habitable? (Macmillan, 1907).

  5. 5.

    Lyot, B. Recherches sur la Polarisation de la Lumière des Planètes et de quelques Substances Terrestres. Thesis, Observatoire de Paris (1929).

  6. 6.

    Pettit, E. & Nicholson, S. B. Lunar radiation and temperatures. Astrophys. J. 71, 102–135 (1930).

  7. 7.

    Wildt, R. On the possible existence of formaldehyde in the atmosphere of Venus. Astrophys. J. 92, 247–255 (1940).

  8. 8.

    Sagan, C. & Kellogg, W. W. The terrestrial planets. Annu. Rev. Astron. Astrophys. 1, 235–266 (1963).

  9. 9.

    Shoemaker, E. M., Hackman, R. J. & Eggleton, R. E. Interplanetary correlation of geologic time. Adv. Astronaut. Sci. 8, 70–89 (1963).

  10. 10.

    Sharp, R. P. & Malin, M. C. Channels on Mars. Geol. Soc. Am. Bull. 86, 593–609 (1975).

  11. 11.

    Sharp, R. P. Geomorphological processes on terrestrial planetary surfaces. Annu. Rev. Earth Planet. Sci. 8, 231–261 (1980).

  12. 12.

    Lovelock, J. E. A physical basis for life detection experiments. Nature 207, 568–570 (1965).

  13. 13.

    Turco, R. P. et al. Nuclear winter: Global consequences of multiple nuclear explosions. Science 222, 1283–1292 (1983).

  14. 14.

    Ingersoll, A. P. The runaway greenhouse: A history of water on Venus. J. Atmos. Sci. 26, 1191–1198 (1969).

  15. 15.

    Winn, J. N. & Fabrycky, D. C. The occurrence and architecture of exoplanetary systems. Annu. Rev. Astron. Astrophys. 53, 409–447 (2015).

  16. 16.

    Morbidelli, A. & Raymond, S. N. Challenges in planet formation. J. Geophys. Res. Planets 121, 1962–1980 (2016).

  17. 17.

    Petigura, E. A., Howard, A. W. & Marcy, G. W. Prevalence of Earth-size planets orbiting Sun-like stars. Proc. Natl Acad. Sci. USA 110, 19273–19278 (2013).

  18. 18.

    Jontof-Hutter, D. The compositional diversity of low-mass exoplanets. Annu. Rev. Earth Planet. Sci. 47, 141–171 (2019).

  19. 19.

    Tarduno, J. A. et al. Geodynamo, solar wind, and magnetopause 3.4 to 3.45 billion years ago. Science 327, 1238–1240 (2010).

  20. 20.

    Biggin, A. J. et al. Palaeomagnetic field intensity variations suggest Mesoproterozoic inner-core nucleation. Nature 526, 245–248 (2015).

  21. 21.

    Driscoll, P. & Bercovici, D. On the thermal and magnetic histories of Earth and Venus: Influences of melting, radioactivity, and conductivity. Phys. Earth Planet. Inter. 236, 36–51 (2014).

  22. 22.

    Labrosse, S. Thermal evolution of the core with a high thermal conductivity. Phys. Earth. Planet. Inter. 247, 36–55 (2015).

  23. 23.

    Olson, P. The new core paradox. Science 342, 431–432 (2013).

  24. 24.

    Davies, C., Pozzo, M., Gubbins, D. & Alfè, D. Constraints from material properties on the dynamics and evolution of Earth’s core. Nat. Geosci. 8, 678–685 (2015).

  25. 25.

    Tang, F. et al. Secondary magnetite in ancient zircon precludes analysis of a Hadean geodynamo. Proc. Natl Acad. Sci. USA 116, 407–412 (2019).

  26. 26.

    Tarduno, J. A. et al. Paleomagnetism indicates that primary magnetite in zircon records a strong Hadean geodynamo. Proc. Natl Acad. Sci. USA 117, 2309–2318 (2020).

  27. 27.

    Cauley, P. W., Shkolnik, E. L., Llama, J. & Lanza, A. F. Magnetic field strengths of hot Jupiters from signals of star–planet interactions. Nat. Astron. 3, 1128–1134 (2019).

  28. 28.

    Driscoll, P. E. in Handbook of Exoplanets (eds Deeg, H. J. & Belmonte, J. A.) 1–18 (Springer, 2018).

  29. 29.

    Jacobson, S. A., Rubie, D. C., Hernlund, J., Morbidelli, A. & Nakajima, M. Formation, stratification, and mixing of the cores of Earth and Venus. Earth Planet. Sci. Lett. 474, 375–386 (2017).

  30. 30.

    Acuña, N. H. et al. Global distribution of crustal magnetization discovered by the Mars Global Surveyor MAG/ER experiment. Science 284, 790–793 (1999).

  31. 31.

    Williams, J.-P. & Nimmo, F. Thermal evolution of the Martian core: Implications for an early dynamo. Geology 32, 97–100 (2004).

  32. 32.

    Weiss, B. P. & Tikoo, S. M. The lunar dynamo. Science 346, 1246753 (2014).

  33. 33.

    Laneuville, M. et al. A long-lived lunar dynamo powered by core crystallization. Earth Planet. Sci. Lett. 401, 251–260 (2014).

  34. 34.

    Le Reun, T. & Le Bars, M. in Fluid Mechanics of Planets and Stars Vol. 595 (eds Le Bars, M. & Leoanet, D.) 91–127 (Springer, 2020).

  35. 35.

    Reddy, K. S., Favier, B. & Le Bars, M. Turbulent kinematic dynamos in ellipsoids driven by mechanical forcing. Geophys. Res. Lett. 45, 1741–1750 (2018).

  36. 36.

    Andrault, D., Monteux, J., Le Bars, M. & Samuel, H. The deep Earth may not be cooling down. Earth Planet. Sci. Lett. 443, 195–203 (2016).

  37. 37.

    Scheinberg, A. L., Soderlund, K. M. & Elkins-Tanton, L. T. A basal magma ocean dynamo to explain the early lunar magnetic field. Earth Planet. Sci. Lett. 492, 144–151 (2018).

  38. 38.

    Scipioni, R., Stixrude, L. & Desjarlais, M. P. Electrical conductivity of SiO2 at extreme conditions and planetary dynamos. Proc. Natl Acad. Sci. USA 114, 9009–9013 (2017).

  39. 39.

    Holmström, E., Stixrude, L., Scipioni, R. & Foster, A. S. Electronic conductivity of solid and liquid (Mg, Fe)O computed from first principles. Earth Planet. Sci. Lett. 490, 11–19 (2018).

  40. 40.

    Labrosse, S., Hernlund, J. W. & Coltice, N. A crystallizing dense magma ocean at the base of the Earth’s mantle. Nature 450, 866–869 (2007).

  41. 41.

    Laneuville, M., Hernlund, J., Labrosse, S. & Guttenberg, N. Crystallization of a compositionally stratified basal magma ocean. Phys. Earth. Planet. Inter. 276, 86–92 (2018).

  42. 42.

    Evans, A. J., Tikoo, S. M. & Andrews-Hanna, J. C. The case against an early lunar dynamo powered by core convection. Geophys. Res. Lett. 45, 98–107 (2018).

  43. 43.

    Bartetzko, A., Delius, H., & Pechnig, R. in Petrophysical Properties of Crystalline Rocks (eds Harvey, P. K., Brewer, T. S., Pezard, P. A. & Petrov, V. A.) 255–278 (Geological Society, 2005).

  44. 44.

    Ziegler, L. B. & Stegman, D. R. Implications of a long-lived basal magma ocean in generating Earth’s ancient magnetic field. Geochem. Geophys. Geosyst. 14, 4735–4742 (2013).

  45. 45.

    O’Rourke, J. G. & Stevenson, D. J. Powering Earth’s dynamo with magnesium precipitation from the core. Nature 529, 387–389 (2016).

  46. 46.

    Badro, J. et al. Magnesium partitioning between Earth’s mantle and core and its potential to drive an early exsolution geodynamo. Geophys. Res. Lett. 45, 13240–13248 (2018).

  47. 47.

    Badro, J., Siebert, J. & Nimmo, F. An early geodynamo by exsolution of mantle components from Earth’s core. Nature 536, 326–328 (2016).

  48. 48.

    Hirose, K. et al. Crystallization of silicon dioxide and compositional evolution of the Earth’s core. Nature 543, 99–102 (2017).

  49. 49.

    Nimmo, F. Why does Venus lack a magnetic field? Geology 30, 987–990 (2002).

  50. 50.

    O’Rourke, J. G., Gillmann, C. & Tackley, P. Prospects for an ancient dynamo and modern crustal remanent magnetism on Venus. Earth Planet. Sci. Lett. 502, 46–56 (2018).

  51. 51.

    Elkins-Tanton, L. T. Linked magma ocean solidification and atmospheric growth for Earth and Mars. Earth Planet. Sci. Lett. 271, 181–191 (2008).

  52. 52.

    Zahnle, K., Schaefer, L. K. & Fegley, B. Jr Earth’s earliest atmosphere. CSH Perspect. Biol. 2, a004895 (2010).

  53. 53.

    Kruijer, T. S., Kleine, T. & Borg, L. E. The great isotopic dichotomy of the early Solar System. Nat. Astron. 4, 32–40 (2020).

  54. 54.

    Braukmüller, N., Wombacher, F., Funk, C. & Münker, C. Earth’s volatile element depletion pattern inherited from a carbonaceous chondrite-like source. Nat. Geosci. 12, 564–568 (2019).

  55. 55.

    Schaefer, L. & Fegley, B. Jr Chemistry of atmospheres formed during accretion of the Earth and other terrestrial planets. Icarus 208, 438–448 (2010).

  56. 56.

    Lebrun, T. et al. Thermal evolution of an early magma ocean in interaction with the atmosphere. J. Geophys. Res. Planets 118, 1155–1176 (2013).

  57. 57.

    Hamno, K., Yutaka, A. & Genda, H. Emergence of two types of terrestrial planet on solidification of magma ocean. Nature 497, 607–610 (2013).

  58. 58.

    Lupu, R. E. et al. The atmospheres of earthlike planets after giant impact events. Astrophys. J. 784, 27 (2014).

  59. 59.

    Demory, B.-O. et al. A map of the large day–night temperature gradient of a super-Earth exoplanet. Nature 532, 207–209 (2016).

  60. 60.

    Ito, Y. et al. Theoretical emission spectra of atmospheres of hot rocky super-Earths. Astrophys. J. 801, 144 (2015).

  61. 61.

    Fegley, B. et al. Solubility of rock in steam atmospheres of planets. Astrophys. J. 824, 103 (2016).

  62. 62.

    Schaefer, L., Wordsworth, R. D., Berta-Thompson, Z. & Sasselov, D. Predictions of the atmospheric composition of GJ 1132b. Astrophys. J. 829, 63 (2016).

  63. 63.

    McKay, C. P., Pollack, J. B. & Courtin, R. The greenhouse and antigreenhouse effects on Titan. Science 253, 1118–1121 (1991).

  64. 64.

    Wordsworth, R. D. & Pierrehumbert, R. Hydrogen-nitrogen greenhouse warming in Earth’s early atmosphere. Science 339, 64–67 (2013).

  65. 65.

    Domagal-Goldman, S. D., Kasting, J. F., Johnston, D. T. & Farquhar, J. Organic haze, glaciations and multiple sulfur isotopes in the Mid-Archean Era. Earth Planet. Sci. Lett. 269, 29–40 (2008).

  66. 66.

    Wolf, E. T. & Toon, O. B. Fractal organic hazes provided an ultraviolet shield for early Earth. Science 328, 1266–1268 (2010).

  67. 67.

    Goldblatt, C. et al. Nitrogen-enhanced greenhouse warming on early Earth. Nat. Geosci. 2, 891–896 (2009).

  68. 68.

    Som, S. M., Catling, D. C., Harnmeijer, J. P., Polivka, P. M. & Buick, R. Air density 2.7 billion years ago limited to less than twice modern levels by fossil raindrop imprints. Nature 484, 359–362 (2012).

  69. 69.

    Wordsworth, R. D. & Pierrehumbert, R. Abiotic oxygen-dominated atmospheres on terrestrial habitable zone planets. Astrophys. J. Lett. 785, L20 (2014).

  70. 70.

    Kleinhböhl, A., Willacy, K., Friedson, A. J., Chen, P. & Swain, M. R. Buildup of abiotic oxygen and ozone in moist atmospheres of temperate terrestrial exoplanets and its impact on the spectral fingerprint in transit observations. Astrophys. J. 862, 92 (2018).

  71. 71.

    Meadows, V. S. et al. Exoplanet biosignatures: Understanding oxygen as a biosignature in the context of its environment. Astrobiology 18, 630–662 (2018).

  72. 72.

    Som, S. M. et al. Earth’s air pressure 2.7 billion years ago constrained to less than half of modern levels. Nat. Geosci. 9, 448–451 (2016).

  73. 73.

    Tomkins, A. G. et al. Ancient micrometeorites suggestive of an oxygen-rich Archaean upper atmosphere. Nature 533, 235–238 (2016).

  74. 74.

    Zahnle, K. & Buick, R. Atmospheric science: Ancient air caught by shooting stars. Nature 533, 184–186 (2016).

  75. 75.

    Rimmer, P. B., Shorttle, O. & Rugheimer, S. Oxidised micrometeorites as evidence for low atmospheric pressure on the early Earth. Geochem. Perspect. Lett. 9, 38–42 (2019).

  76. 76.

    Johnson, B. & Goldblatt, C. The nitrogen budget of Earth. Earth-Sci. Rev. 148, 150–173 (2015).

  77. 77.

    Wordsworth, R. D. Atmospheric nitrogen evolution on Earth and Venus. Earth Planet. Sci. Lett. 447, 103–111 (2016).

  78. 78.

    Clapham, M. E. & Renne, P. R. Flood basalts and mass extinctions. Annu. Rev. Earth Planet. Sci. 47, 275–303 (2019).

  79. 79.

    Palmer, K. F. & Williams, D. Optical constants of sulfuric acid; application to the clouds of Venus? Appl. Opt. 14, 208–219 (1975).

  80. 80.

    Rossow, W. B. Cloud microphysics: analysis of the clouds of Earth, Venus, Mars and Jupiter. Icarus 36, 1–50 (1978).

  81. 81.

    Bullock, M. A. & Grinspoon, D. H. The recent evolution of climate on Venus. Icarus 150, 19–37 (2001).

  82. 82.

    Halevy, I. & Head, J. W. III Episodic warming on early Mars by punctuated volcanism. Nat. Geosci. 7, 865–868 (2014).

  83. 83.

    Pope, K. O., Baines, K. H., Ocampo, A. C. & Ivanov, B. A. Impact winter and the Cretaceous/Tertiary extinctions: results of a Chicxulub asteroid impact model. Earth Planet. Sci. Lett. 128, 719–725 (1994).

  84. 84.

    Pope, K. O., Baines, K. H., Ocampo, A. C. & Ivanov, B. A. Energy, volatile production, and climatic effects of the Chicxulub Cretaceous/Tertiary impact. J. Geophys. Res. Planets 102, 21645–21664 (1997).

  85. 85.

    Timmreck, C. et al. Aerosol size confines climate response to volcanic super-eruptions. Geophys. Res. Lett. 37, L24705 (2010).

  86. 86.

    Macdonald, F. A. & Wordsworth, R. Initiation of Snowball Earth with volcanic sulfur aerosol emissions. Geophys. Res. Lett. 44, 1938–1946 (2017).

  87. 87.

    Keith, D. W. & MacMartin, D. G. A temporary, moderate and responsive scenario for solar geoengineering. Nat. Clim. Change 5, 201–206 (2015).

  88. 88.

    Ribas, I., Guinan, E. F., Güdel, M. & Audard, M. Evolution of the solar activity over time and effects on planetary atmospheres. I. High-energy irradiances (1-1700 Å). Astrophys. J. 622, 680 (2005).

  89. 89.

    Claire, M. W. et al. The evolution of solar flux from 0.1 nm to 160 µm: Quantitative estimates for planetary studies. Astrophys. J. 757, 95 (2012).

  90. 90.

    Zahnle, K. J. & Walker, J. C. G. The evolution of solar ultraviolet luminosity. Rev. Geophys. 20, 280–292 (1982).

  91. 91.

    Tu, L., Johnstone, C. P., Güdel, M. & Lammer, H. The extreme ultraviolet and X-ray Sun in Time: high-energy evolutionary tracks of a solar-like star. Astron. Astrophys. 577, L3 (2015).

  92. 92.

    van Hunen, J. & Moyen, J.-F. Archean subduction: fact or fiction? Annu. Rev. Earth Planet. Sci. 40, 195–219 (2012).

  93. 93.

    Korenaga, J. Initiation and evolution of plate tectonics on Earth: theories and observations. Annu. Rev. Earth Planet. Sci. 41, 117–151 (2013).

  94. 94.

    McKinnon, W. B., Zhanle, K. J., Ivanov, B. D. & Melosh, J. H. in Venus II (eds Bougher, S. W., Hunten, D. M. & Philips, R. J.) (Univ. Arizona Press, 1997).

  95. 95.

    Hansen, V. L. Global tectonic evolution of Venus, from exogenic to endogenic over time, and implications for early Earth processes. Phil. Trans. R. Soc. A 376, 20170412 (2018).

  96. 96.

    Davaille, A., Smrekar, S. E. & Tomlinson, S. Experimental and observational evidence for plume-induced subduction on Venus. Nat. Geosci. 10, 349–355 (2017).

  97. 97.

    Gilmore, M., Treiman, A., Helbert, J. & Smrekar, S. E. Venus surface composition constrained by observation and experiment. Space Sci. Rev. 212, 1511–1540 (2017).

  98. 98.

    Campbell, I. H. & Taylor, S. R. No water, no granites–no oceans, no continents. Geophys. Res. Lett. 10, 1061–1064 (1983).

  99. 99.

    Hartmann, W. K. & Neukum, G. Cratering chronology and the evolution of Mars. Space Sci. Rev. 96, 165–194 (2001).

  100. 100.

    Ehlmann, B. L. et al. The sustainability of habitability on terrestrial planets: Insights, questions, and needed measurements from Mars for understanding the evolution of Earth-like worlds. J. Geophys. Res. Planets 121, 1927–1961 (2016).

  101. 101.

    Banham, S. G. et al. Ancient Martian aeolian processes and palaeomorphology reconstructed from the Stimson formation on the lower slope of Aeolis Mons, Gale crater, Mars. Sedimentology 65, 993–1042 (2018).

  102. 102.

    Williams, R. M. E. et al. Martian fluvial conglomerates at Gale crater. Science 340, 1068–1072 (2013).

  103. 103.

    Grotzinger, J. P. et al. A habitable fluvio-lacustrine environment at Yellowknife Bay, Gale crater, Mars. Science 343, 1242777 (2014).

  104. 104.

    Stack, K. M. et al. Evidence for plunging river plume deposits in the Pahrump Hills member of the Murray formation, Gale crater, Mars. Sedimentology 66, 1768–1802 (2019).

  105. 105.

    Ohtomo, Y., Kakegawa, T., Ishida, A., Nagase, T. & Rosing, M. T. Evidence for biogenic graphite in early Archaean Isua metasedimentary rocks. Nat. Geosci. 7, 25–28 (2014).

  106. 106.

    Tashiro, T. et al. Early trace of life from 3.95 Ga sedimentary rocks in Labrador, Canada. Nature 549, 516–518 (2017).

  107. 107.

    Dietrich, W. E. & Perron, J. T. The search for a topographic signature of life. Nature 439, 411–418 (2006).

  108. 108.

    Gurnell, A. Plants as river system engineers. Earth Surf. Process Landf. 39, 4–25 (2014).

  109. 109.

    Glibling, M. R. et al. Palaeozoic co-evolution of rivers and vegetation: a synthesis of current knowledge. Proc. Geol. Assoc. 125, 524–533 (2014).

  110. 110.

    McMahon, W. J. & Davies, N. S. Evolution of alluvial mudrock forced by early land plants. Science 359, 994–995 (2018).

  111. 111.

    Burr, D. M., Williams, R. M. E., Wendell, K. D., Chojnacki, M. & Emery, J. P. Inverted fluvial features in the Aeolis/Zephyria Plana region, Mars: formation mechanism and initial paleodischarge estimates. J. Geophys. Res. Planets 115, E07011 (2010).

  112. 112.

    Williams, R. M., Irwin, R. P. III, Burr, D. M., Harrison, T. & McClelland, P. Variability in Martian sinuous ridge form: case study of Aeolis Serpens in the Aeolis Dorsa, Mars, and insight from the Mirackina paleoriver, South Australia. Icarus 225, 308–324 (2013).

  113. 113.

    Lapôtre, M. G. A., Ielpi, A., Lamb, M. P., Williams, R. M. E. & Knoll, A. H. Model for the formation of single-thread rivers in barren landscapes and implications for pre-Silurian and Martian fluvial deposits. J. Geophys. Res. Earth Surf. 124, 2757–2777 (2019).

  114. 114.

    Ielpi, A. & Lapôtre, M. G. A. A tenfold slowdown in river meander migration driven by plant life. Nat. Geosci. 13, 82–86 (2020).

  115. 115.

    Torres, M. A. et al. Model predictions of long-lived storage of organic carbon in river deposits. Earth Surf. Dyn. 5, 711–730 (2017).

  116. 116.

    Hazen, R. M. et al. Mineral evolution. Am. Mineral. 93, 1693–1720 (2008).

  117. 117.

    Adcock, C. T., Hausrath, E. M. & Forster, P. M. Readily available phosphate from minerals in early aqueous environments on Mars. Nat. Geosci. 6, 824–827 (2013).

  118. 118.

    Sasselov, D. D., Grotzinger, J. P. & Sutherland, J. D. The origin of life as a planetary phenomenon. Sci. Adv. 6, eaax3419 (2020).

  119. 119.

    Schaefer, L. & Sasselov, D. The persistence of oceans on Earth-like planets: Insights from the deep-water cycle. Astrophys. J. 801, 40 (2015).

  120. 120.

    Walker, J. C. G., Hays, P. B. & Kasting, J. F. A negative feedback mechanism for the long-term stabilization of Earth’s surface temperature. J. Geophys. Res. Oceans 86, 9776–9782 (1981).

  121. 121.

    Checlair, J. H. et al. A statistical comparative planetology approach to maximize the scientific return of future exoplanet characterization efforts. arXiv (2019).

  122. 122.

    Greenwood, J. P., Karato, S.-I., Vander Kaaden, K. E., Pahlevan, K. & Usui, T. Water and volatile inventories of Mercury, Venus, the Moon, and Mars. Space Sci. Rev. 214, 92 (2018).

  123. 123.

    Hirth, G. & Kohlstedt, D. L. Water in the oceanic upper mantle: implications for rheology, melt extraction and the evolution of the lithosphere. Earth Planet. Sci. Lett. 144, 93–108 (1996).

  124. 124.

    Korenaga, J., Planavsky, N. J. & Evans, D. A. Global water cycle and the coevolution of the Earth’s interior and surface environment. Philos. Trans. R. Soc. A 375, 20150393 (2017).

  125. 125.

    Fei, H., Wiedenbeck, M., Yamakazi, D. & Katsura, T. Small effect of water on upper-mantle rheology based on silicon self-diffusion coefficients. Nature 498, 213–215 (2013).

  126. 126.

    Mackwell, S. J., Zimmerman, M. E. & Kohlstedt, D. L. High-temperature deformation of dry diabase with application to tectonics on Venus. J. Geophys. Res. Solid Earth 103, 975–984 (1998).

  127. 127.

    Montési, L. G. J. Fabric development as the key for forming ductile shear zones and enabling plate tectonics. J. Struct. Geol. 50, 254–266 (2013).

  128. 128.

    Tikoo, S. M. & Elkins-Tanton, L. T. The fate of water within Earth and super-Earths and implications for plate tectonics. Philos. Trans. R. Soc. A 375, 20150394 (2017).

  129. 129.

    Kasting, J. F. & Pollack, J. B. Loss of water from Venus. I. Hydrodynamic escape of hydrogen. Icarus 53, 479–508 (1983).

  130. 130.

    Kurosawa, K. Impact-driven planetary desiccation: The origin of the dry Venus. Earth Planet. Sci. Lett. 429, 181–190 (2015).

  131. 131.

    Foley, B. J., Bercovici, D. & Landuyt, W. The conditions for plate tectonics on super-Earths: Inferences from convection models with damage. Earth Planet. Sci. Lett. 331–332, 281–290 (2012).

  132. 132.

    Robinson, T. D. et al. Detection of ocean glint and ozone absorption using LCROSS Earth observations. Astrophys. J. 787, 171 (2014).

  133. 133.

    de Wit, J. et al. A combined transmission spectrum of the Earth-sized exoplanets TRAPPIST-1b and c. Nature 537, 69–72 (2016).

  134. 134.

    Bourrier, V. et al. Temporal evolution of the high-energy irradiation and water content of TRAPPIST-1 exoplanets. Astron. J. 154, 121 (2017).

  135. 135.

    Kane, S. R. et al. Venus as a laboratory for exoplanetary science. J. Geophys. Res. Planets 124, 2015–2028 (2019).

  136. 136.

    Bean, J. L., Abbot, D. S. & Kempton, E. M. R. A statistical comparative planetology approach to the hunt for habitable exoplanets and life beyond the solar system. Astrophys. J. Lett. 841, L24 (2017).

  137. 137.

    Lamb, M. P., Grotzinger, J. P., Southard, J. B. & Tosca, N. J. in Sedimentary Geology of Mars Vol. 102 (eds Grotzinger, J. P. & Milliken, R. E.) 139–150 (Society for Sedimentary Geology, 2012).

  138. 138.

    Lapôtre, M. G. A. et al. Large wind ripples on Mars: a record of atmospheric evolution. Science 353, 55–58 (2016).

  139. 139.

    Burr, D. M. et al. Fluvial features on Titan: insights from morphology and modeling. Bull. Geol. Soc. Am. 125, 299–321 (2013).

  140. 140.

    Telfer, M. W. et al. Dunes on Pluto. Science 360, 992–997 (2018).

  141. 141.

    Jia, P., Andreotti, B. & Claudin, P. Giant ripples on comet 67P/Churyumov–Gerasimenko sculpted by sunset thermal wind. Proc. Natl Acad. Sci. USA 114, 2509–2514 (2017).

  142. 142.

    Grotzinger, J. P. et al. in Comparative Climatology of Terrestrial Planets (eds. Mackwell, S. J., Bullock, M. A. & Harder, J. W.) 99–123 (Univ. Arizona Press, 2013).

  143. 143.

    Thomas, N. et al. The morphological diversity of comet 67P/Churyumov-Gerasimenko. Science 347, aaa0440 (2015).

  144. 144.

    Ewing, R. C. et al. Sedimentary processes of the Bagnold Dunes: implications for the eolian rock record of Mars. J. Geophys. Res. Planets 122, 2544–2573 (2017).

  145. 145.

    Lapôtre, M. G. A. et al. Morphologic diversity of Martian ripples: Implications for large-ripple formation. Geophys. Res. Lett. 45, 10229–10239 (2018).

  146. 146.

    Siminovich, A. et al. Numerical study of shear stress distribution over sand ripples under terrestrial and Martian conditions. J. Geophys. Res. Planets 124, 175–185 (2019).

  147. 147.

    Duran Vinent, O., Andreotti, B., Claudin, P. & Winter, C. A unified model of ripples and dunes in water and planetary environments. Nat. Geosci. 12, 345–350 (2019).

  148. 148.

    Lapôtre, M. G. A., Lamb, M. P. & McElroy, B. What sets the size of current ripples? Geology 45, 243–246 (2017).

  149. 149.

    Kok, J. F. Difference in the wind speeds required for initiation versus continuation of sand transport on Mars: Implications for dunes and dust storms. Phys. Rev. Lett. 104, 074502 (2010).

  150. 150.

    Sullivan, R. et al. Results of the Imager for Mars Pathfinder windsock experiment. J. Geophys. Res. Planets 105, 24547–24562 (2000).

  151. 151.

    Bridges, N. T. et al. Martian aeolian activity at the Bagnold Dunes, Gale Crater: The view from the surface and orbit. J. Geophys. Res. Planets 122, 2077–2110 (2017).

  152. 152.

    Newman, C. E. et al. Winds measured by the Rover Environmental Monitoring Station (REMS) during the Mars Science Laboratory (MSL) rover’s Bagnold Dunes Campaign and comparison with numerical modeling using MarsWRF. Icarus 291, 203–231 (2017).

  153. 153.

    Bridges, N. T. et al. Planet-wide sand motion on Mars. Geology 40, 31–34 (2012).

  154. 154.

    Bridges, N. T. et al. Earth-like sand fluxes on Mars. Nature 485, 339–342 (2012).

  155. 155.

    Sullivan, R. et al. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at “El Dorado” and surroundings at Gusev Crater. J. Geophys. Res. Planets 113, E06S07 (2008).

  156. 156.

    Baker, M. M. et al. Coarse sediment transport in the modern Martian environment. J. Geophys. Res. Planets 123, 1380–1394 (2018).

  157. 157.

    Baker, M. M. et al. The Bagnold Dunes in southern summer: active sediment transport on Mars observed by the Curiosity rover. Geophys. Res. Lett. 45, 8853–8863 (2018).

  158. 158.

    Kok, J. F. An improved parameterization of wind-blown sand flux on Mars that includes the effect of hysteresis. Geophys. Res. Lett. 37, L12202 (2010).

  159. 159.

    Yizhaq, H., Kok, J. F. & Katra, I. Basaltic sand ripples at Eagle crater as indirect evidence for the hysteresis effect in Martian saltation. Icarus 230, 143–150 (2014).

  160. 160.

    Sullivan, R. & Kok, J. F. Aeolian saltation on Mars at low wind speeds. J. Geophys. Res. Planets 122, 2111–2143 (2017).

  161. 161.

    Fedo, C. M., McGlynn, I. O. & McSween, H. Y. Jr. Grain size and hydrodynamic sorting controls on the composition of basaltic sediments: Implications for interpreting Martian soils. Earth Planet. Sci. Lett. 423, 67–77 (2015).

  162. 162.

    Siebach, K. L. et al. Sorting out compositional trends in sedimentary rocks of the Bradbury group (Aeolis Palus), Gale crater, Mars. J. Geophys. Res. Planets 122, 295–328 (2017).

  163. 163.

    Lapôtre, M. G. A. et al. Compositional variations in sands of the Bagnold Dunes, Gale Crater, Mars, from visible-shortwave infrared spectroscopy and comparison with ground truth from the Curiosity rover. J. Geophys. Res. Planets 122, 2489–2509 (2017).

  164. 164.

    Ehlmann, B. L. et al. Chemistry, mineralogy, and grain properties at Namib and High dunes, Bagnold dune field, Gale crater, Mars: A synthesis of Curiosity rover observations. J. Geophys. Res. Planets 122, 2510–2543 (2017).

  165. 165.

    Rampe, E. B. et al. Sand mineralogy within the Bagnold Dunes, Gale crater, as observed in situ and from orbit. Geophys. Res. Lett. 45, 9488–9497 (2018).

  166. 166.

    Huang, J. et al. An ALMA survey of DCN/H13CN and DCO+/H13CO+ in protoplanetary disks. Astrophys. J. 835, 231 (2017).

  167. 167.

    Walsh, K. J., Morbidelli, A., Raymond, S. N., O’Brien, D. P. & Mandell, A. M. A low mass for Mars from Jupiter’s early gas-driven migration. Nature 475, 206–209 (2011).

  168. 168.

    Spalding, C. The primordial solar wind as a sculptor of terrestrial planet formation. Astrophys. J. Lett. 869, L17 (2018).

  169. 169.

    Dong, C. et al. Atmospheric escape from the TRAPPIST-1 planets and implications for habitability. Proc. Natl Acad. Sci. USA 115, 260–265 (2018).

  170. 170.

    Daly, R. A. Meteorites and an earth-model. Bull. Geol. Soc. Am. 54, 401–456 (1943).

  171. 171.

    Patterson, C., Tilton, G. & Inghram, M. Age of the Earth. Science 121, 65–75 (1955).

  172. 172.

    Suess, H. E. & Urey, H. C. Abundances of the elements. Rev. Mod. Phys. 28, 53–74 (1956).

  173. 173.

    Wood, J. A. On the origin of chondrules and chondrites. Icarus 2, 152–180 (1963).

  174. 174.

    Clayton, R. N., Onuma, N. & Mayeda, T. K. A classification of meteorites based on oxygen isotopes. Earth Planet. Sci. Lett. 30, 10–18 (1976).

  175. 175.

    Hart, S. R. & Zindler, A. In search of a bulk-Earth composition. Chem. Geol. 57, 247–267 (1986).

  176. 176.

    Allègre, C. J., Manhès, G. & Göpel, C. The age of the Earth. Geochim. Cosmochim. Acta 59, 1445–1456 (1995).

  177. 177.

    Amelin, Y., Krot, A. N., Hutcheon, I. D. & Ulyanov, A. A. Lead isotopic ages of chondrules and calcium-aluminum-rich inclusions. Science 297, 1678–1683 (2002).

  178. 178.

    Dauphas, N. The isotopic nature of the Earth’s accreting material through time. Nature 541, 521–524 (2017).

  179. 179.

    Gänsicke, B. T. et al. The chemical diversity of exo-terrestrial planetary debris around white dwarfs. Mon. Not. R. Astron. Soc. 424, 333–347 (2012).

  180. 180.

    Fitzsimmons, A. et al. Detection of CN gas in interstellar object 2I/Borisov. Astrophys. J. Lett. 885, L9 (2019).

  181. 181.

    Doyle, A. E., Young, E. D., Klein, B., Zuckerman, B. & Schlichting, H. E. Oxygen fugacities of extrasolar rocks: evidence for an Earth-like geochemistry of exoplanets. Science 366, 356–359 (2019).

  182. 182.

    Bergin, E. A., Blake, G. A., Ciesla, F., Hirschmann, M. M. & Li, J. Tracing the ingredients for a habitable Earth from interstellar space through planet formation. Proc. Natl Acad. Sci. USA 112, 8965–8970 (2015).

  183. 183.

    Seligman, D. & Laughlin, G. The feasibility and benefits of in situ exploration of ‘Oumuamua-like objects. Astron. J. 155, 217 (2018).

  184. 184.

    Jacobsen, S. B. The Hf-W isotopic system and the origin of the Earth and Moon. Annu. Rev. Earth Planet. Sci. 33, 531–570 (2005).

  185. 185.

    Nemchin, A. et al. Timing of crystallization of the lunar magma ocean constrained by the oldest zircon. Nat. Geosci. 2, 133–136 (2009).

  186. 186.

    Barboni, M. et al. Early formation of the Moon 4.51 billion years ago. Sci. Adv. 3, e1602365 (2017).

  187. 187.

    Elkins-Tanton, L. T., Burgess, S. & Yin, Q.-Z. The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology. Earth Planet. Sci. Lett. 304, 326–336 (2011).

  188. 188.

    Bottke, W. F. & Norman, M. D. The late heavy bombardment. Annu. Rev. Earth Planet. Sci. 45, 619–647 (2017).

  189. 189.

    Marchi, S. et al. Widespread mixing and burial of Earth’s Hadean crust by asteroid impact. Nature 511, 578–582 (2014).

  190. 190.

    Wetherill, G. W. Late heavy bombardment of the Moon and the terrestrial planets. Proc. 6th Lunar Science Conf. Vol. 2, 1539–1561 (1975).

  191. 191.

    Boehnke, P. & Harrison, T. M. Illusory late heavy bombardment. Proc. Natl Acad. Sci. USA 113, 10802–10806 (2016).

  192. 192.

    Bellucci, J. J. et al. Terrestrial-like zircon in a clast from an Apollo 14 breccia. Earth Planet. Sci. Lett. 510, 173–185 (2019).

  193. 193.

    Hoyle, F. Remarks on the computation of evolutionary tracks. Ric. Astron. 5, 223–230 (1958).

  194. 194.

    Sagan, C. & Mullen, G. Earth and Mars: Evolution of atmospheres and surface temperatures. Science 177, 52–56 (1972).

  195. 195.

    Sagan, C. & Chyba, C. The early faint sun paradox: organic shielding of ultraviolet-labile greenhouse gases. Science 276, 1217–1221 (1997).

  196. 196.

    Haqq-Misra, J. D., Domagal-Goldman, S. D., Kasting, P. J. & Kasting, J. F. A revised, hazy methane greenhouse for the Archean Earth. Astrobiology 8, 1127–1137 (2008).

  197. 197.

    Feulner, G. The faint young Sun problem. Rev. Geophys. 50, RG2006 (2012).

  198. 198.

    Spalding, C. & Fischer, W. W. A shorter Archean day-length biases interpretations of the early Earth’s climate. Earth Planet. Sci. Lett. 514, 28–36 (2019).

  199. 199.

    Bowen, G. H. & Willson, L. A. Large early solar mass loss – 1. Solar system evolution. Meteoritics 21, 338–339 (1986).

  200. 200.

    Wood, B. E., Müller, H. R., Redfield, S. & Edelman, E. Evidence for a weak wind from the young Sun. Astrophys. J. Lett. 781, L33 (2014).

  201. 201.

    Guzik, J. A. & Mussack, K. Exploring mass loss, low-Z accretion, and convective overshoot in solar models to mitigate the solar abundance problem. Astrophys. J. 713, 1108 (2010).

  202. 202.

    Wood, S. R., Mussack, K. & Guzik, J. A. Solar models with dynamic screening and early mass loss tested by helioseismic, astrophysical, and planetary constraints. Sol. Phys. 293, 111 (2018).

  203. 203.

    Oran, R., Weiss, B. P. & Cohen, O. Were chondrites magnetized by the early solar wind? Earth Planet. Sci. Lett. 492, 222–231 (2018).

  204. 204.

    Fu, R. R. et al. Solar nebula magnetic fields recorded in the Semarkona meteorite. Science 346, 1089–1092 (2014).

  205. 205.

    Minton, D. A. & Malhotra, R. Assessing the massive young Sun hypothesis to solve the warm young Earth puzzle. Astrophys. J. 660, 1700–1706 (2007).

  206. 206.

    Spalding, C., Fischer, W. W. & Laughlin, G. An orbital window into the ancient Sun’s mass. Astrophys. J. Lett. 869, L19 (2018).

  207. 207.

    Lewis, K. W. et al. Quasi-periodic bedding in the sedimentary record of Mars. Science 322, 1532–1535 (2008).

  208. 208.

    Stack, K. M., Grotzinger, J. P. & Milliken, R. E. Bed thickness distributions on Mars: An orbital perspective. J. Geophys. Res. Planets 118, 1323–1349 (2013).

  209. 209.

    Beaty, D. W. et al. The potential science and engineering value of samples delivered to Earth by Mars sample return. Meteorit. Planet. Sci. 54, S3–S152 (2019).

  210. 210.

    Canup, R. M. Simulations of a late lunar-forming impact. Icarus 168, 433–456 (2004).

  211. 211.

    Lock, S. J. et al. The origin of the moon within a terrestrial synestia. J. Geophys. Res. Planets 123, 910–951 (2018).

  212. 212.

    Gardner, J. P. et al. The James Webb space telescope. Space Sci. Rev. 123, 485–606 (2006).

  213. 213.

    McComas, D. J. et al. Probing the energetic particle environment near the Sun. Nature 576, 223–227 (2019).

  214. 214.

    Cournede, C. et al. An early solar system magnetic field recorded in CM chondrites. Earth Planet. Sci. Lett. 410, 62–74 (2015).

  215. 215.

    Hoffman, J. H., Hodges, R. R., Donahue, T. M. & McElroy, M. B. Composition of the Venus lower atmosphere from the Pioneer Venus Mass Spectrometer. J. Geophys. Res. Space 85, 7882–7890 (1980).

  216. 216.

    Chassefière, E., Wieler, R., Marty, B. & Leblanc, F. The evolution of Venus: present state of knowledge and future exploration. Planet. Space Sci. 63–64, 15–23 (2012).

  217. 217.

    Zeng, L. et al. Growth model interpretation of planet size distribution. Proc. Natl Acad. Sci. USA 116, 9723–9728 (2019).

  218. 218.

    Tasker, E. et al. The language of exoplanet ranking metrics needs to change. Nat. Astron. 1, 0042 (2017).

  219. 219.

    Rogers, L. A. Most 1.6 Earth-radius planets are not rocky. Astrophys. J. 801, 41 (2015).

  220. 220.

    Filiberto, J., Trang, D., Treiman, A. H. & Gilmore, M. S. Present-day volcanism on Venus as evidenced from weathering rates of olivine. Sci. Adv. 6, eaax7445 (2020).

  221. 221.

    Strom, R., Schaber, G. & Dawson, D. The global resurfacing of Venus. J. Geophys. Res. Planets 99, 10899–10926 (1994).

  222. 222.

    Herrick, R. R. & Rumpf, M. E. Postimpact modification by volcanic or tectonic processes as the rule, not the exception, for Venusian craters. J. Geophys. Res. Planets 116, E02004 (2011).

  223. 223.

    Smrekar, S. E. et al. Recent hotspot volcanism on Venus from VIRTIS emissivity data. Science 328, 605–608 (2010).

  224. 224.

    Esposito, L. W. et al. Sulfur dioxide at the Venus cloud tops, 1978–1986. J. Geophys. Res. Atmos. 93, 5267–5276 (1988).

  225. 225.

    Donahue, T. M., Hoffman, J. H., Hodges, R. R. & Watson, A. J. Venus was wet: A measurement of the ratio of deuterium to hydrogen. Science 216, 630–633 (1982).

  226. 226.

    Greeley, R. et al. Aeolian features on Venus: preliminary Magellan results. J. Geophys. Res. Planets 97, 13319–13345 (1992).

  227. 227.

    Radebaugh, J. et al. Dunes on Titan observed by Cassini radar. Icarus 194, 690–703 (2008).

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We thank the reviewers for their insightful and constructive suggestions, which helped us improve this manuscript.

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Lapôtre, M.G.A., O’Rourke, J.G., Schaefer , L.K. et al. Probing space to understand Earth. Nat Rev Earth Environ 1, 170–181 (2020).

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