A simple chondritic model of Mars

Sanloup, C.; Jambon, Albert; Gillet, Ph.

doi:10.1016/s0031-9201(98)00175-7

Cited by 210 publications

(252 citation statements)

References 34 publications

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“…[5] We conclude here that it is unlikely that Mars has significantly sub-chondritic abundances of U, Th, and K. On the other hand, strong spatial variations in heat flow occur in convecting systems, and we show that our existing models of mantle plume magmatism on Mars [Li and Kiefer, 2007] [Wänke and Dreibus, 1994;Lodders and Fegley, 1997;Sanloup et al, 1999;Mohapatra and Murty, 2003;Agee and Draper, 2004]. Abundances in Table 1 are for the bulk silicate planet, assuming that all of the K, U, and Th partition into the silicates and using the published silicate fraction for each model.…”

Section: Introductionmentioning

confidence: 70%

Mantle convection controls the observed lateral variations in lithospheric thickness on present‐day Mars

Kiefer

2009

Geophysical Research Letters

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Sounding radar observations of the north polar layered deposits on Mars suggest an elastic lithosphere thickness of at least 300 km in that region, significantly larger than any prior estimate of lithospheric thickness on Mars. Previous studies interpreted this result as requiring either that Mars is significantly sub‐chondritic in its abundance of radioactive elements, or alternatively that there are large lateral variations in lithospheric thickness. We find that the required depletion of radioactivity is geochemically unlikely. On the other hand, stagnant lid convection naturally produces factor of two or more lateral variations in both mantle heat flux and lithospheric thickness and is the preferred explanation for the polar elastic thickness measurement. Our mantle plume models, which have previously been shown to explain observations of present‐day magma production on Mars, can also explain the new elastic thickness observations.

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Section: Introductionmentioning

confidence: 70%

Mantle convection controls the observed lateral variations in lithospheric thickness on present‐day Mars

Kiefer

2009

Geophysical Research Letters

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“…A composition of 3.5-16 wt.% S is estimated in the Martian core based on the geochemical constraints [Morgan and Anders, 1979;Dreibus and Wänke, 1985;Sanloup et al, 1999], whereas O content in the core was not mentioned. If the core-forming melt has approximately 3.5 wt.% S, little amount of oxygen may be included by equilibrium in the magma ocean because of the low solubility of O in the metallic melt even at high temperatures.…”

Section: Resultsmentioning

confidence: 99%

In situ observation and determination of liquid immiscibility in the Fe‐O‐S melt at 3 GPa using a synchrotron X‐ray radiographic technique

Tsuno¹,

Terasaki²,

Ohtani³

et al. 2007

Geophysical Research Letters

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We have performed in situ experiments on liquid immiscibility in Fe‐O‐S melts at 3 GPa and up to 2203 K using a synchrotron X‐ray radiographic technique. The difference between immiscible melts and a miscible melt can be clearly observed in radiographs. The immiscibility gap of the Fe‐O‐S melt shrinks with increasing temperature at 3 GPa. Two separated phases appeared from a miscible melt during quenching. Without in situ observations, the two phases observed in quench textures would be interpreted as either quench products from primary immiscible melts at high temperature, or those exsolved from a homogeneous melt to immiscible melts passing through the stability field of immiscible melts during quenching. In situ measurements are required in order to determine the immiscibility gap of the liquid Fe with light element(s). Our results have important implications for the formation and chemical composition of the cores of Earth and Mars.

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“…These models are based on both geochemical Wanke, 1984, 1985;Lodders and Fegley Jr., 1997;Morgan and Anders, 1979;Sanloup et al, 1999) and geophysical arguments (Khan and Connolly, 2008). They converge towards a single composition that displays key differences from the bulk silicate Earth: lower Mg# (75-78) and higher incompatible (Na, K, P) and compatible (Cr, Mn) volatile elements (Table 1).…”

Section: The Primitive Mantle Of Marsmentioning

confidence: 99%

“…We selected the composition from the model of Dreibus and Wanke (1984) for a number of reasons: (1) it is based on comparisons between shergottites and CI chondrites with carefully chosen ratios of elements that behave similarly in magmatic systems; (2) of all the geochemical models, it is the closest to the physically constrained composition of Khan and Connolly (2008); (3) while enriched in volatile elements relative to the bulk silicate Earth, it is characterized by less extreme alkali contents than other models (Lodders and Fegley Jr., 1997;Sanloup et al, 1999) and provides a composition of the primitive mantle after the potential syn-accretion volatile depletion (Albarede, 2009;Halliday and Porcelli, 2001); (4) it is similar to compositions used for earlier experimental studies of the melting of the martian mantle (Agee and Draper, 2004;Holloway, 1994a, 1994b;Matsukage et al, 2013), allowing direct comparisons. (Holloway et al, 1992;Médard et al, 2008).…”

Section: The Primitive Mantle Of Marsmentioning

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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A simple chondritic model of Mars

Cited by 210 publications

References 34 publications

Mantle convection controls the observed lateral variations in lithospheric thickness on present‐day Mars

Mantle convection controls the observed lateral variations in lithospheric thickness on present‐day Mars

In situ observation and determination of liquid immiscibility in the Fe‐O‐S melt at 3 GPa using a synchrotron X‐ray radiographic technique

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

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