The early differentiation history of Mars from 182W-142Nd isotope systematics in the SNC meteorites

By C. Foley, M. Wadhwa, L. Borg, P. Janney, R. Hines, T. Grove. 2005

180 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/2788625fe33d3b128681d2d557f8c7bd87dcd2b4

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Citations in the corpus

What Martian Meteorites Reveal About the Interior and Surface of Mars (2020, background): “Nakhlites and chassignites have the same depleted radiogenic isotopic compositions, with high (142)Nd/(144)Nd, and (182)W/(184)W, and low (87)Sr/(86)Sr, but these compositions are distinct from shergottites (Carlson & Boyet, 2009; Caro et al., 2008; Debaille et al., 2009; Foley et al., 2005; Nyquist”
Bulk composition and early differentiation of Mars (2007, background): “The nakhlites appear to derive from yet a third source region [ Foley et al., 2005 ].”
A review of lunar chronology revealing a preponderance of 4.34–4.37 Ga ages (2015, background): “…variation in e142Nd in lunar samples is very small compared to other solar system bodies, such as Mars (Harper et al. 1995; Borg et al. 1997, 2003; Foley et al. 2005; Debaille et al. 2007; Caro et al. 2008), the eurcite parent body (Wadhwa and Lugmair 1996), or the angrite parent body (Lugmair…”
Emergence of a Habitable Planet (2007, background): “The most recent data for martian meteorites (Kleine et al. 2004; Foley et al. 2005) confirms earlier evidence (Lee and Halliday 1997) that accretion and core formation on Mars were fast.”
Magma oceans in the inner solar system (2012, background): “Foley et al. (2005) further proposed that the Martian mantle differentiated into source reservoirs for the shergottite and nakhlite meteorite compositions within ∼60 Ma (and perhaps as little as 20 Ma) of the first solar system solids.”
Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, methodology): “In the second model, the NC source formed at the same time as the shergottite source(s) and in this case the NC must have evolved with very high 180Hf/184W 56 and 147Sm/144Nd 0.303 to reach their present-day e182W and e142Nd values (e.g., Foley et al., 2005).”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, methodology): “The best tool to investigate this question is the radionuclide 182Hf, which decays to 182W with a t1/2 of 8.9 Myr (Figure 5; see also Dauphas & Pourmand 2011; Foley et al. 2005; Jacobsen 2005; Kleine et al. 2007, 2009; Lee & Halliday 1997; Nimmo & Kleine 2007).”
The composition of Mars (2019, background): “et al., 2012; McSween, 2015). Furthermore, radiogenic isotope systematics of nakhlites and chassignites indicate a third reservoir which was moderately depleted in incompatible elements (Jones, 2003; Foley et al., 2005; Treiman, 2005; McCubbin et al., 2013; Day et al., 2018; Udry and Day, 2018). Low”
The age of SNC meteorites and the antiquity of the Martian surface (2005, background): “although more pronounced than in shergottites [ 16 ].”
Water and astrobiology (2007, background): “Mars probably formed and differentiated its core within the first million years (Halliday and Kleine, 2006) (although Foley et al. (2005) estimate 12Myr).”