Stable-isotopic anomalies and the accretionary assemblage of the Earth and Mars: A subordinate role for carbonaceous chondrites

By P. Warren. 2011

643 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology, Geophysics

View Paper: https://www.semanticscholar.org/paper/dfbccd8568f4a873d764016427f60d7aac93cd39

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Citations in the corpus

The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, methodology): “1), then the Earth may have incorporated a much larger amount of CC material of up to ∼ 40–50% (Schiller et al. 2018; Warren 2011).”
The Compositional Structure of the Asteroid Belt (2015, background): “Similarly, only one achondrite, the ungrouped basaltic achondrite NWA 011and several paired specimens from the same fall, seems to have formed by melting of a carbonaceous chondrite-like body (Warren, 2011).”
Populating the asteroid belt from two parent source regions due to the migration of giant planets—“The Grand Tack” (2012, background): “These physical differences are not easily accounted for in a cooling nebula (Warren 2011) and therefore origin at different locations in the disk is a potential solution.”
The composition of Mars (2019, background): “, O, Ni, Cr, Ti, Mo, W) are now clearly established for the non-carbonaceous and carbonaceous (NC and CC, respectively) meteorite groups, including the chondrites (Warren, 2011; Dauphas and Schauble, 2016; Kruijer et al., 2017a).”
Calcium-48 isotopic anomalies in bulk chondrites and achondrites: Evidence for a uniform isotopic reservoir in the inner protoplanetary disk (2014, background): “A similar weak correlation (not shown) exists between ε48Ca or ε50Ti, and ε54Cr for achondrites, ordinary chondrites and enstatite chondrites but carbonaceous chondrites fall off this trend (Trinquier et al., 2007, 2009; Qin et al., 2010; Warren, 2011; Zhang et al., 2012).”
Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies (2017, background): “10) (Warren, 2011b) (Section 3.2.3).”
Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk (2012, background): “However, the initial 60 Fe/ 56 Fe ratio at the time of solar system formation is highly uncertain with estimates that span over two orders of magnitude (Birck and Lugmair, 1988; Shukolyukov and Lugmair, 1993a, b; Tachibana et al., 2003, 2006; Mostefaoui et al., 2004; 2005; Sugiura et al., 2006; Quit”