Early martian mantle overturn inferred from isotopic composition of nakhlite meteorites

Debaille, Vinciane; Brandon, A. D.; O’Neill, Craig; Yin, Qing‐Zhu; Jacobsen, Ben

doi:10.1038/ngeo579

Cited by 101 publications

(129 citation statements)

References 31 publications

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“…The compositions of other martian rocks are from Agee et al (2013), Humayun et al (2013), McSween et al (2006b, Ming et al (2008) and Stolper et al (2013). a magma ocean (Debaille et al, 2009;Elkins-Tanton et al, 2005;Scheinberg et al, 2014). Another possibility, which could be related to the former, is that the mantle source of Columbia Hills rocks was re-fertilized by variable amounts of low-degree melts.…”

Section: Columbia Hills: Alkali Basaltsmentioning

confidence: 99%

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Collinet

Médard

Charlier

et al. 2015

Earth and Planetary Science Letters

109

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We have performed piston-cylinder experiments on a primitive martian mantle composition between 0.5 and 2.2 GPa and 1160 to 1550 • C. The composition of melts and residual minerals constrain the possible melting processes on Mars at 50 to 200 km depth under nominally anhydrous conditions. Silicate melts produced by low degrees of melting (<10 wt.%) were analyzed in layers of vitreous carbon spheres or in micro-cracks inside the graphite capsule. The total range of melt fractions investigated extends from 5 to 50 wt.%, and the liquids produced display variable SiO 2 (43.7-59.0 wt.%), MgO (5.3-18.6 wt.%) and Na 2 O + K 2 O (1.0-6.5 wt.%) contents. We provide a new equation to estimate the solidus temperature of the martian mantle: T ( • C) = 1033 + 168.1P (GPa) − 14.22P 2 (GPa), which places the solidus 50 • C below that of fertile terrestrial peridotites. Low-and high-degree melts are compared to martian alkaline rocks and basalts, respectively. We suggest that the parental melt of Adirondack-class basalts was produced by ∼25 wt.% melting of the primitive martian mantle at 1.5 GPa (∼135 km) and ∼1400 • C. Despite its brecciated nature, NWA 7034/7533 might be composed of material that initially crystallized from a primary melt produced by ∼10-30 wt.% melting at the same pressure. Other igneous rocks from Mars require mantle reservoirs with different CaO/Al 2 O 3 and FeO/MgO ratios or the action of fractional crystallization. Alkaline rocks can be derived from mantle sources with alkali contents (∼0.5 wt.%) similar to the primitive mantle.

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Section: Columbia Hills: Alkali Basaltsmentioning

confidence: 99%

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Collinet

Médard

Charlier

et al. 2015

Earth and Planetary Science Letters

109

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“…Wadhwa and Crozaz (1995) argued that the REE in nakhlites evolved as a closed system, however, making post-crystallization addition of LREE-enriched fluids unlikely. Debaille et al (2009) 143 Nd systematics of the SNC meteorites provide clear evidence for differentiation of the Martian mantle in the first few ten to hundred Ma after solar system formation, the exact timescale of magma ocean solidification remains uncertain and depends on the differentiation model and bulk Sm-Nd isotope composition assumed for Mars. Either the shergottites witness a major single-event crystallization of the magma ocean at 47 ± 12 Ma after solar system formation Foley et al 2005;Caro et al 2008), or a protracted shallow magma ocean that finished crystallizing ∼ 90 Ma after solar system formation (Debaille et al 2007).…”

Section: Duration Of a Martian Magma Oceanmentioning

confidence: 99%

“…The Hf-W systematics of the nakhlites rather seem to indicate an early Hf/W fractionation in a garnet-bearing source (Righter and Shearer 2003;Kleine et al 2004aKleine et al , 2004bFoley et al 2005). Recently, Debaille et al (2009) 143 Nd and 182 Hf-182 W systematics. These authors argued that the combined Hf-Nd isotope systematics of the nakhlites require segregation of garnet/majoritic garnet from their source and proposed the following model evolution (Fig.…”

Section: Magma Ocean Crystallization and Cumulate Overturnmentioning

confidence: 99%

“…(Caro et al 2008;Caro and Bourdon 2010). Data from Debaille et al (2007), Caro et al (2008), Debaille et al (2009) The 142 Nd record of the nakhlites is even more difficult to interpret than that of the shergottites. The elevated 142 Nd/ 144 Nd ratio of the nakhlites corresponds to a twostage model age of ∼25 Ma after CAI formation (Harper et al 1995;Foley et al 2005).…”

Section: Duration Of a Martian Magma Oceanmentioning

confidence: 99%

“…However, the nakhlites plot outside the two-stage evolutionary field in the 142 Nd vs. 143 Nd diagram (Fig. 5), indicating that the two-stage model ages might be meaningless and that a more complex model may be required to constrain the age of the nakhlite source Debaille et al 2009). The 146 Nd systematics of the nakhlites are similar to those of the depleted shergottites, whereas the 147 Sm-143 Nd systematics reveal differences.…”

Section: Duration Of a Martian Magma Oceanmentioning

confidence: 99%

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Core Formation and Mantle Differentiation on Mars

Mezger¹,

Debaille²,

Kleine³

2012

Quantifying the Martian Geochemical Reservoirs

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Geochemical investigation of Martian meteorites (SNC meteorites) yields important constraints on the chemical and geodynamical evolution of Mars. These samples may not be representative of the whole of Mars; however, they provide constraints on the early differentiation processes on Mars. The bulk composition of Martian samples implies the presence of a metallic core that formed concurrently as the planet accreted. The strong depletion of highly siderophile elements in the Martian mantle is only possible if Mars had a large scale magma ocean early in its history allowing efficient separation of a metallic melt from molten silicate. The solidification of the magma ocean created chemical heterogeneities whose ancient origin is manifested in the heterogeneous 142 Nd and 182 W abundances observed in different meteorite groups derived from Mars. The isotope anomalies measured in SNC meteorites imply major chemical fractionation within the Martian mantle during the life time of the short-lived isotopes 146 Sm and 182 Hf. The Hf-W data are consistent with very rapid accretion of Mars within a few million years or, alternatively, a more protracted accretion history involving several large impacts and incomplete metal-silicate equilibration during core formation. In contrast to Earth early-formed chemical heterogeneities are still preserved on Mars, albeit slightly modified by mixing processes. The preservation of such ancient chemical differences is only possible if Mars did not undergo efficient whole mantle convection or vigorous plate tectonic style processes after the first few tens of millions of years of its history. K. Mezger ( )

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Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile‐rich igneous source

et al. 2014

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[1] The first four rocks examined by the Mars Science Laboratory Alpha Particle X-ray Spectrometer indicate that Curiosity landed in a lithologically diverse region of Mars. These rocks, collectively dubbed the Bradbury assemblage, were studied along an eastward traverse (sols 46-102). Compositions range from Na-and Al-rich mugearite Jake_Matijevic to Fe-, Mg-, and Zn-rich alkali-rich basalt/hawaiite Bathurst_Inlet and span nearly the entire range in FeO* and MnO of the data sets from previous Martian missions and Martian meteorites. The Bradbury assemblage is also enriched in K and moderately volatile metals (Zn and Ge). These elements do not correlate with Cl or S, suggesting that they are associated with the rocks themselves and not with salt-rich coatings. Three out of the four Bradbury rocks plot along a line in elemental variation diagrams, suggesting mixing between Al-rich and Fe-rich components. ChemCam analyses give insight to their degree of chemical heterogeneity and grain size. Variations in trace elements detected by ChemCam suggest chemical weathering (Li) and concentration in mineral phases (e.g., Rb and Sr in feldspars). We interpret the Bradbury assemblage to be broadly volcanic and/or volcaniclastic, derived either from near the Gale crater rim and transported by the Peace Vallis fan network, or from a local volcanic source within Gale Crater. High Fe and Fe/Mn in Et_Then likely reflect secondary precipitation of Fe 3+ oxides as a cement or rind. The K-rich signature of the Bradbury assemblage, if igneous in origin, may have formed by small degrees of partial melting of metasomatized mantle. , et al. (2014), Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile-rich igneous source,

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Early martian mantle overturn inferred from isotopic composition of nakhlite meteorites

Cited by 101 publications

References 31 publications

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Core Formation and Mantle Differentiation on Mars

Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile‐rich igneous source

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