Constraining the early evolution of Venus and Earth through atmospheric Ar, Ne isotope and bulk K/U ratios

Lämmer, H.; Leitzinger, M.; Scherf, Manuel; Odert, P.; Burger, Christoph; Kubyshkina, Daria; Johnstone, C. P.; Maindl, Thomas I.; Schäfer, Christoph; Güdel, M.; Tosi, Nicola; Nikolaou, Athanasia; Marcq, Emmanuel; Еркаев, Н. В.; Noack, Lena; Kislyakova, K. G.; Fossati, L.; Pilat-Lohinger, Elke; Ragossnig, Florian; Dorfi, E. A.

doi:10.1016/j.icarus.2019.113551

Cited by 67 publications

(91 citation statements)

References 161 publications

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“…Within our model framework, Earth reaches 60% of its current mass at the dissipation of the protoplanetary disc after 5 Ma. This mass of the proto-Earth agrees well with constraints from matching the 36 Ar/ 8 Ar, 20 Ne/ 22 Ne, and 36 Ar/ 22 Ne ratios by drag from the hydrodynamic escape of the primordial hydrogen/helium envelope ( 47 ). We augment the mass of Earth with the introduction of an additional planet Theia (40% Earth mass) between the orbits of Earth and Mars, to later collide with Earth to form our Moon.…”

Section: Discussionsupporting

confidence: 82%

“…For Earth, the envelope temperature lies above the 2600 K of silicate sublimation close to the planetary core. This high surface temperature will lead to extensive melting of the protoplanet and to the formation of a magma ocean of at least 1000 km in depth ( 47 ). Our Mars analog does not reach silicate melting temperatures at the surface, but trapped heat released by 26 Al within the protoplanet could heat the interior above the melting temperature.…”

Section: Resultsmentioning

confidence: 99%

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A pebble accretion model for the formation of the terrestrial planets in the Solar System

et al. 2021

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Pebbles of millimeter sizes are abundant in protoplanetary discs around young stars. Chondrules inside primitive meteorites—formed by melting of dust aggregate pebbles or in impacts between planetesimals—have similar sizes. The role of pebble accretion for terrestrial planet formation is nevertheless unclear. Here, we present a model where inward-drifting pebbles feed the growth of terrestrial planets. The masses and orbits of Venus, Earth, Theia (which later collided with Earth to form the Moon), and Mars are all consistent with pebble accretion onto protoplanets that formed around Mars’ orbit and migrated to their final positions while growing. The isotopic compositions of Earth and Mars are matched qualitatively by accretion of two generations of pebbles, carrying distinct isotopic signatures. Last, we show that the water and carbon budget of Earth can be delivered by pebbles from the early generation before the gas envelope became hot enough to vaporize volatiles.

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Section: Discussionsupporting

confidence: 82%

Section: Resultsmentioning

confidence: 99%

A pebble accretion model for the formation of the terrestrial planets in the Solar System

et al. 2021

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“…Prior to this time, a higher mixing ratio of CO 2 or another greenhouse gas serving as an upper atmosphere coolant was likely necessary to protect the atmosphere from rapid thermal escape. This result is in agreement with climate studies (Feulner, 2012), studies of the thermal escape and on isotope fractionation (Lammer et al., 2020), and with geological evidences (Catling & Zahnle, 2020).…”

Section: Resultssupporting

confidence: 90%

“…The amount of short‐wavelength radiation a star produces is tightly linked to its rotational evolution, with stars born as fast rotators emitting more XUV radiation and likely having stronger winds than stars born as slow rotators. Although the investigation of the Sun's early history is far from being complete, there exist some indications that the Sun was born as a slow rotator (Lammer et al., 2020).…”

Section: Introductionmentioning

confidence: 99%

Evolution of the Earth's Polar Outflow From Mid‐Archean to Present

et al. 2020

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The development of habitable conditions on Earth is tightly connected to the evolution of its atmosphere, which is strongly influenced by atmospheric escape. We investigate the evolution of the polar ion outflow from the open field line bundle, which is the dominant escape mechanism for the modern Earth. We perform Direct Simulation Monte Carlo (DSMC) simulations and estimate the upper limits on escape rates from the Earth's open field line bundle starting from 3 gigayears ago (Ga) to present assuming the present‐day composition of the atmosphere. We perform two additional simulations with lower mixing ratios of oxygen of 1% and 15% to account for the conditions shortly after the Great Oxydation Event (GOE). We estimate the maximum loss rates due to polar outflow 3 gigayears ago of 3.3×1027 s−1 and 2.4×1027 s−1 for oxygen and nitrogen, respectively. The total integrated mass loss equals to 39% and 10% of the modern atmosphere's mass, for oxygen and nitrogen, respectively. According to our results, the main factors that governed the polar outflow in the considered time period are the evolution of the XUV radiation of the Sun and the atmosphere's composition. The evolution of the Earth's magnetic field plays a less important role. We conclude that although the atmosphere with the present‐day composition can survive the escape due to polar outflow, a higher level of CO2 between 3.0 and 2.0 Ga was likely necessary to reduce the escape.

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“…A challenge for numerical simulations is the low density of an atmosphere compared with the planet, which requires high resolution (Kegerreis et al 2019). For this reason, previous studies have made progress by focusing primarily on 1D models or thick atmospheres (> ∼ 5% of the total mass), often also limited to only head-on impacts or too few scenarios to make broad scaling predictions (Genda & Abe 2005;Inamdar & Schlichting 2015;Hwang et al 2018;Denman et al 2020;Lammer et al 2020). Kegerreis et al (2020, hereafter K20) used high-resolution smoothed particle hydrodynamics (SPH) simulations of giant impacts to investigate the detailed dependence of atmospheric loss on the speed and angle of an impact and to examine the different mechanisms by which thin atmospheres could be eroded.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric Erosion by Giant Impacts onto Terrestrial Planets: A Scaling Law for any Speed, Angle, Mass, and Density

Kegerreis

Eke

Catling

et al. 2020

ApJL

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Constraining the early evolution of Venus and Earth through atmospheric Ar, Ne isotope and bulk K/U ratios

Cited by 67 publications

References 161 publications

A pebble accretion model for the formation of the terrestrial planets in the Solar System

A pebble accretion model for the formation of the terrestrial planets in the Solar System

Evolution of the Earth's Polar Outflow From Mid‐Archean to Present

Atmospheric Erosion by Giant Impacts onto Terrestrial Planets: A Scaling Law for any Speed, Angle, Mass, and Density

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