Linked magma ocean solidification and atmospheric growth for Earth and Mars

By L. Elkins‐Tanton. 2008

524 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/22c1ae32f3dfee886f968f665f53e83a4d8f6aae

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Citations in the corpus

The sulfur content of volcanic gases on Mars (2009, methodology): “H volatile content ([Elkins-Tanton, 2008] and [Hirschmann and Withers, 2008]), and with a sulfur content based on the above estimate for the martian mantle (900 ppm, Fig.”
Thermal evolution of an early magma ocean in interaction with the atmosphere (2012, unknown): “…phases, where M s perov and M s lherz are, respectively, the masses of the solid phases for perovskite and lherzolite, k vol perov the partition coefﬁcient of volatile (H 2 O or CO 2 ) for perovskite, and k vol lherz the partition coefﬁ-cient for lherzolite (see Table 3) [ Elkins-Tanton , 2008].”
Evidence for multiple magma ocean outgassing and atmospheric loss episodes from mantle noble gases (2013, background): “Magma ocean outgassing can efficiently transfer volatiles (e.g., N2, H2O, and CO2) from the mantle to the exosphere (Elkins-Tanton, 2008; Zahnle et al., 2007).”
Magma oceans in the inner solar system (2012, methodology): “In contrast, if the magma ocean is not sufficiently reducing to stabilize graphite, carbon species dominate the degassing budget and the emissivity of the atmosphere (Elkins-Tanton 2008).”
FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES (2011, methodology): “We model the H2O in a differentiated water layer surrounding the mantle, although in practice some water may be sequestered into the silicates (e.g., Elkins-Tanton 2008, and references therein).”
Origin and loss of nebula-captured hydrogen envelopes from ‘sub’- to ‘super-Earths’ in the habitable zone of Sun-like stars (2014, background): “…from the luminosity generated by accretion, it is also reasonable to assume that the planetary core stores a fraction of the internal energy generated in the formation process (Elkins-Tanton 2008; Hamano et al. 2013) which is a quite recent event, in any case for a planet in the nebula phase.”
Gravity Recovery and Interior Laboratory (GRAIL): Mapping the Lunar Interior from Crust to Core (2013, background): “For example, while the Moon was once thought to be unique in developing a “magma ocean” shortly after accretion (Wood et al. 1970), such a phenomenon has now been credibly proposed for Mars as well (Elkins-Tanton 2008).”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “…the lifetime of a magma ocean, since the released greenhouse volatiles exert a blanketing effect that can significantly delay solidification (e.g. Abe and Matsui 1985; ZaHnle et al. 1988; Abe 1997; Elkins-Tanton 2008; Lebrun et al 2013; Hamano et al. 2013; Massol et al. 2016; Salvador et al. 2017).”
Crustal evolution and the temporality of anorthosites (2017, background): “Although it seems likely that a terrestrial magma ocean formed during Earth accretion (Abe, 1997; Elkins-Tanton, 2008), none of its products have yet been recognized.”
A theoretical framework for volcanic degassing chemistry in a comparative planetology perspective and implications for planetary atmospheres (2014, background): “types of processes fueling secondary atmospheres are illustrated, including the Magma Ocean stage (Elkins-Tanton, 2008; Gaillard and Scaillet, 2009; Hirschmann, 2012), which progressively shift ed to volcanic eruptions emitting gas equilibrat ed under moderately oxidized conditions (Gaillard and Sca”
THREE POSSIBLE ORIGINS FOR THE GAS LAYER ON GJ 1214b (2009, background): “We consider Fe (ǫ) (Anderson et al. 2001), Mg1−χFeχSiO3 perovskite (Elkins-Tanton 2008), and H2O ice (Hemley et al. 1987).”
Melting and mixing states of the Earth’s mantle after the Moon-forming impact (2015, background): “In addition to the mantle mixing, understanding the extent of the impact-induced mantle melting is important because the extent affected the evolution of the Earth’s interior and atmosphere (e.g., Abe and Matsui, 1986; Tonks and Melosh, 1993; Elkins-Tanton, 2008).”
The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology (2011, methodology): “Compositions of mineral phases are calculated in equilibrium with the magma ocean liquid composition at that stage of solidification, using experimentally determined KDs for major elements and partition coefficients for trace elements; see Elkins-Tanton (2008).”
The Evaporation Valley in the Kepler Planets (2017, background): “…least a few percent of H/He envelopes (“water-worlds” with water/steam envelopes are ruled out), this amount of gas lies above the most optimistic estimate for outgassing (Elkins-Tanton 2008; Elkins-Tanton & Seager 2008) and suggests that the envelopes were accreted from the protoplanetary discs.”