Loss and Fractionation of Noble Gas Isotopes and Moderately Volatile Elements from Planetary Embryos and Early Venus, Earth and Mars

Lämmer, H.; Scherf, Manuel; Kurokawa, Hiroyuki; Ueno, Yuichiro; Burger, Christoph; Maindl, Thomas I.; Johnstone, C. P.; Leizinger, Martin; Benedikt, Markus; Fossati, L.; Kislyakova, K. G.; Marty, Bernard; Avice, Guillaume; Fegley, B.; Odert, P.

doi:10.1007/s11214-020-00701-x

Cited by 49 publications

(74 citation statements)

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“…In the case that proto-Earth accreted higher amounts of carbonaceous chondritic material compared to the 2% inferred from today's data (Marty, 2012), thermal processing in a possible primordial atmosphere and atmospheric escape from accreting planetary embryos and the growing protoplanet could have been depleted in these volatile elements (Odert et al, 2018;Benedikt et al, 2019;Young et al, 2019;Lammer et al, 2020a, this issue;2020b), altering the bulk and isotopic composition. In early Earth's case, today's atmospheric 36 Ar/ 22 Ne ratio of 18.8 (Marty and Allé, 1994;Marty, 2012) can be best reproduced by Lammer et al (2020a;2020b) if the post-nebula impactors (0.15 -0.3 MEarth) contain roughly 5% carbonaceous chondritic material (see Fig. 5; dashed lines) if one assumes an initial composition as suggested by Dauphas (2017), and ≥ 70% (see Fig.…”

Section: 12) Becausementioning

confidence: 99%

“…Evolution scenario that reproduces present Earth's atmospheric 20 Ne/ 22 Ne, 36 Ar/ 38 Ar and 36 Ar/ 22 Ne ratios and the corresponding early mass accretion of proto-Earth as modelled by Lammer et al (2020a) with a proto-Earth-mass at 4 Myr of 0.55 MEarth, a small captured H2-dominated primordial atmosphere that is lost within < 7 Myr after the origin of the Solar System, and ≈ 3 Myr after disk dispersal due to impact erosion and EUV-driven hydrodynamic escape related to a young Sun that rotates slower than a moderate rotator. Case 1: Reproduction of Earth's atmospheric 20 Ne/ 22 Ne, 36 Ar/ 38 Ar and 36 Ar/ 22 Ne ratios if one assumes the initial composition given in Dauphas (2017), but with a CC contribution of about 5 % after a tiny primordial atmosphere escaped (see also Sect.…”

Section: Figmentioning

confidence: 99%

“…On the other hand, one can expect that Earth's deep mantle should also be depleted in 3 He in a similar way as the other volatiles, because of volatile depletion in proto-Earth's nebula source reservoir, metamorphic degassing in planetesimals, as well as degassing from large planetesimals and planetary embryos during accretion (Harper and Jacobsen, 1996;Jacobsen et al, 2008;Lichtenberg et al, 2016;2018;Benedikt et al, 2020;Lammer et al, 2020a, this issue).…”

Section: Constraining Early Earth's Accretion Bymentioning

confidence: 99%

“…By applying the same assumption as Ikoma and Genda (2006) for an accretion scenario that can reproduce the present day atmospheric Ar and Ne isotope ratios based on the simulations of Lammer et al (2020a), a proto-Earth with a mass of 0.55 MEarth (see also Fig. 5) with a captured primordial H-dominated atmosphere of roughly MH2 ≈ 3.5 × 10 -5 MEarth (or 2.15 × 10 20 kg) produces a water reservoir of MH2O of ≈ 3.0 × 10 19 g from the H2-envelope corresponding to only ≈ 2% of the current value of Earth's seawater (see Fig.…”

Section: Containing Early Earth's Accretion From D/hmentioning

confidence: 99%

“…As illustrated in Fig. 1, depending on their speed of growth before or after disk dissipation and their orbital locations of origin/destination, protoplanets will evolve into objects with different volatile and elemental abundances, which results in different elemental ratios compared to their initial ones due to subsequent atmospheric escape and/or impact erosion of atmospheres and crustal/mantle material (e.g., Lammer et al, 2020a;this issue;O'Neill et al, 2020; this issue). Safronov (1969) proposed the first physical model for the formation of the terrestrial planets.…”

Section: Introductionmentioning

confidence: 99%

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Formation of Venus, Earth and Mars: Constrained by Isotopes

et al. 2020

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Here we discuss the current state of knowledge of terrestrial planet formation from the aspects of different planet formation models and isotopic data from 182 Hf-182 W, U-Pb, lithophile-siderophile elements, 48 Ca/ 44 Ca isotope samples from planetary building blocks, recent reproduction attempts from 36 Ar/ 38 Ar, 20 Ne/ 22 Ne, 36 Ar/ 22 Ne isotope ratios in Venus' and Earth's atmospheres, the expected solar 3 He abundance in Earth's deep mantle and Earth's D/H sea water ratios that shed light on the accretion time of the early protoplanets. Accretion scenarios that can explain the different isotope ratios, including a Moon-forming event ca. 50 Myr after the formation of the Solar System, support the theory that the bulk of Earth's mass (≥ 80 %) most likely accreted within 10-30 Myr. From a combined analysis of the before mentioned isotopes, one finds that proto-Earth accreted a mass of 0.5-0.6 MEarth within the first ≈ 4-5 Myr, the approximate lifetime of the protoplanetary disk. For Venus, the available atmospheric noble gas data are too uncertain for constraining the planet's accretion scenario accurately. However, from the available imprecise Ar and Ne isotope measurements, one finds that proto-Venus could have grown to a mass of 0.85-1.0 MVenus before the disk dissipated. Classical terrestrial planet formation models have struggled to grow large planetary embryos, or even cores of giant planets, quickly from the tiniest materials within the typical lifetime of protoplanetary disks. Pebble accretion could solve this long-standing time scale controversy. Pebble accretion and streaming instabilities produce large planetesimals that grow into Marssized and larger planetary embryos during this early accretion phase. The later stage of accretion can be explained well with the Grand-Tack model as well as the annulus and depleted disk models. The relative roles of pebble accretion and planetesimal accretion/giant impacts are poorly understood and should be investigated with N-body simulations that include pebbles and multiple protoplanets. To summarise, different isotopic dating methods and the latest terrestrial planet formation models indicate that the accretion process from dust settling, planetesimal formation, and growth to large planetary embryos and protoplanets is a fast process that occurred to a great extent in the Solar System within the lifetime of the protoplanetary disk.

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Section: 12) Becausementioning

confidence: 99%

Section: Figmentioning

confidence: 99%

Section: Constraining Early Earth's Accretion Bymentioning

confidence: 99%

Section: Containing Early Earth's Accretion From D/hmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Formation of Venus, Earth and Mars: Constrained by Isotopes

et al. 2020

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Planetary Atmospheres Through Time: Effects of Mass Loss and Thermal Evolution

Kubyshkina

2024

Handbook of Exoplanets

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Future Missions Related to the Determination of the Elemental and Isotopic Composition of Earth, Moon and the Terrestrial Planets

et al. 2020

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In this chapter, we review the contribution of space missions to the determination of the elemental and isotopic composition of Earth, Moon and the terrestrial planets, with special emphasis on currently planned and future missions. We show how these missions are going to significantly contribute to, or sometimes revolutionise, our understanding of planetary evolution, from formation to the possible emergence of life. We start with the Earth, which is a unique habitable body with actual life, and that is strongly related to its atmosphere. The new wave of missions to the Moon is then reviewed, which are going to study its formation history, the structure and dynamics of its tenuous exosphere and the interaction of the Moon’s surface and exosphere with the different sources of plasma and radiation of its environment, including the solar wind and the escaping Earth’s upper atmosphere. Missions to study the noble gas atmospheres of the terrestrial planets, Venus and Mars, are then examined. These missions are expected to trace the evolutionary paths of these two noble gas atmospheres, with a special emphasis on understanding the effect of atmospheric escape on the fate of water. Future missions to these planets will be key to help us establishing a comparative view of the evolution of climates and habitability at Earth, Venus and Mars, one of the most important and challenging open questions of planetary science. Finally, as the detection and characterisation of exoplanets is currently revolutionising the scope of planetary science, we review the missions aiming to characterise the internal structure and the atmospheres of these exoplanets.

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Loss and Fractionation of Noble Gas Isotopes and Moderately Volatile Elements from Planetary Embryos and Early Venus, Earth and Mars

Cited by 49 publications

References 256 publications

Formation of Venus, Earth and Mars: Constrained by Isotopes

Formation of Venus, Earth and Mars: Constrained by Isotopes

Planetary Atmospheres Through Time: Effects of Mass Loss and Thermal Evolution

Future Missions Related to the Determination of the Elemental and Isotopic Composition of Earth, Moon and the Terrestrial Planets

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