The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology

By L. Elkins‐Tanton, S. Burgess, Q. Yin. 2011

491 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/06c8e4a615eeeaae5e6586c0683169f2343c6ba4

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Citations in the corpus

Generation, ascent and eruption of magma on the Moon:new insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted Emplacement Processes and Observations) (2017, background): “1 c), magma ocean cooling and solidification ( Shearer et al., 2006 ) was accompanied by lithospheric stabilization and thickening ( Wieczorek et al., 2006; Elkins-Tanton et al., 2011 ).”
A review of lunar chronology revealing a preponderance of 4.34–4.37 Ga ages (2015, background): “The young ur-KREEP model age could, in principle, reflect late closure of the Sm-Nd and LuHf systems due to tidal heating (Elkins-Tanton et al. 2011; McLeod et al. 2014) or internal heat production due to the decay of Th (Wieczorek and Phillips 2000).”
Crustal evolution and the temporality of anorthosites (2017, background): “Another possibility is that magma ocean solidification, thought to occur on timescales 106 years (Elkins-Tanton et al., 2011), might have been prolonged by thermal insulation of the anorthositic crust (Solomon and Longhi, 1977), due to internal heat production from KREEP (Wieczorek and Phillips,…”
The origin of water in the primitive Moon as revealed by the lunar highlands samples (2014, background): “Estimates of the timing of LMO crystallisation suggest that the entire LMO can solidify within the first 10 Ma and up to 200 Ma after the Moon formation (Elkins-Tanton et al., 2011).”
Magma oceans in the inner solar system (2012, background): “References for ages ( far left) of core formation in iron meteorites, formation of chondrules, and genesis of angrites and eucrites from Elkins-Tanton et al. (2011b) and this review.”
Asymmetric thermal evolution of the Moon (2012, background): “We do not consider stable post-magma ocean overturn temperature profiles here [such as in Hess and Parmentier, 1995; Elkins-Tanton et al., 2011], in an attempt to keep the setting of our model as simple as possible.”
The timeline of the lunar bombardment: Revisited (2018, methodology): “, 2010; Chen and Nimmo, 2013), the ultimate crystallization could have been delayed by up to 100 or even 200 My (Elkins-Tanton et al., 2011).”
Lunar resources (2014, background): “Examples include: (i) an early ‘magma ocean’ phase, when most or all of the Moon appears to have been molten (e.g. Elkins-Tanton et al., 2011); (ii) subsequent production of magnesium-rich magmas and their intrusion into the lunar crust (e.g. Taylor et al., 1991); (iii) thick sequences of impact…”