A model for the thermal and chemical evolution of the Moon's interior: implications for the onset of mare volcanism

Hess, P. C.; Parmentier, E. M.

doi:10.1016/0012-821x(95)00138-3

Cited by 368 publications

(390 citation statements)

References 25 publications

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“…We include the possible effect of gravitational overturn of unstably stratified magma ocean cumulates [cf. Hess and Parmentier, 1995]. This overturn would increase temperatures at shallow depths beneath the residual KREEP by bringing high-temperature Mg-rich cumulates from depth.…”

Section: Thermal Modelmentioning

confidence: 98%

“…Korotev [2000] argued that the crystallization of the last dregs of the magma ocean not only was prolonged but also experienced a renewed thermal activity, which resulted in the remelting of the magnesian cumulates below the crust. The latter appear in that stratigraphic position because of the overturn of the cumulate pile of the magma ocean [Ryder, 1991;Hess and Parmentier, 1995]. Wieczorek and Phillips [2000] predict that the residual KREEP layer remains partially molten for a few billion years and that this layer provides sufficient thermal energy to partially melt the deep interior and produce mare basalts.…”

Section: Introductionmentioning

confidence: 99%

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Thermal evolution of a thicker KREEP liquid layer

Hess¹,

Parmentier²

2001

J. Geophys. Res.

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Abstract. We consider the thermal evolution of the thickened potassium, rare earth element, and phosphorous (KREEP) liquid layer that extends over a significant fraction of the lunar nearside with a prescribed thickness and heat production and beneath an insulating anorthosite crust. This layer represents a subcrustal heat source beneath the Procellarum-Imbrium terrane and may be responsible for the localized and anomalous enrichments of highly incompatible elements in this terrane. In some models this thickened liquid layer is the thermal source for the remelting of mare basalts and also produces the parent magmas of the magnesian suite. Indeed, a KREEP liquid layer thickened from 5 to 10 km with more than 200 times chondritic heat-producing elements does not continue to cool but undergoes a reheating and grows in thickness by dissolving several times its mass of anorthosite and ultramafic cumulates. However, such a liquid layer cannot give rise to the parent magmas to the magnesian suite, because it cannot account for the extraordinarily high incompatible element content, the primitive major element content, or the positive /•nd of the magnesian suite. This growing layer will also form an impenetrable barrier to the eruption of mare basalts and is generally inconsistent with a number of geophysical constraints of the Moon, specifically, the existence of mascons subsequent to the basin filling by mare basalts. A thickened KREEP liquid layer can, however, explain the asymmetry in the distribution of KREEP-rich rock on the lunar crust. Such a KREEP layer must be efficiently cooled and be quickly solidified to avoid some of the difficulties described above. A thinned anorthosite crust would allow efficient heat loss and induce crystallization of such a layer early in lunar history.

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Section: Thermal Modelmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Thermal evolution of a thicker KREEP liquid layer

Hess¹,

Parmentier²

2001

J. Geophys. Res.

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“…This leads to a layered structure of the mantle and to density instability of the cumulate pile (e.g. Hess and Parmentier, 1995;Elkins-Tanton et al, 2003). The cumulate sequence then overturns just after magma ocean solidification ends in order to achieve a stable configuration.…”

Section: Origin Of Compositional Variations Of Surface Terrains On Mementioning

confidence: 99%

Phase equilibria of ultramafic compositions on Mercury and the origin of the compositional dichotomy

Charlier

Grove

Zuber

2013

Earth and Planetary Science Letters

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a b s t r a c tMeasurements of major element ratios obtained by the MESSENGER spacecraft using x-ray fluorescence spectra are used to calculate absolute element abundances of lavas at the surface of Mercury. We discuss calculation methods and assumptions that take into account the distribution of major elements between silicate, metal, and sulfide components and the potential occurrence of sulfide minerals under reduced conditions. These first compositional data, which represent large areas of mixed highreflectance volcanic plains and low-reflectance materials and do not include the northern volcanic plains, share common silica-and magnesium-rich characteristics. They are most similar to terrestrial volcanic rocks known as basaltic komatiites. Two compositional groups are distinguished by the presence or absence of a clinopyroxene component. Melting experiments at one atmosphere on the average compositions of each of the two groups constrain the potential mineralogy at Mercury's surface, which should be dominated by orthopyroxene (protoenstatite and orthoenstatite), plagioclase, minor olivine if any, clinopyroxene (augite), and tridymite. The two compositional groups cannot be related to each other by any fractional crystallization process, suggesting differentiated source compositions for the two components and implying multi-stage differentiation and remelting processes for Mercury. Comparison with high-pressure phase equilibria supports partial melting at pressure o10 kbar, in agreement with last equilibration of the melts close to the crust-mantle boundary with two different mantle lithologies (harzburgite and lherzolite). Magma ocean crystallization followed by adiabatic decompression of mantle layers during cumulate overturn and/or convection would have produced adequate conditions to explain surface compositions. The surface of Mercury is not an unmodified quenched crust of primordial bulk planetary composition. Ultramafic lavas from Mercury have high liquidus temperatures (1450-1350 1C) and very low viscosities, in accordance with the eruption style characterized by flooding of pre-existing impact craters by lava and absence of central volcanoes.

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“…[7] Crystallization of an early magma ocean is believed to have resulted in an ultramafic mantle overlaid by an anorthositic crust [e.g., Wood et al, 1970, Snyder et al, 1992Hess and Parmentier, 1995;Elkins-Tanton et al, 2011]. On average, the crust is~40 km thick, as shown by recent models incorporating Gravity Recovery and Interior Laboratory (GRAIL) gravity and Lunar Orbiter Laser Altimeter (LOLA) topography data [Wieczorek et al, 2013].…”

Section: The Evolution and Stratigraphy Of The Lunar Crust And Mantlementioning

confidence: 99%

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

2013

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[1] Using high-spectral and -spatial resolution Moon Mineralogy Mapper data, we investigate compositional variations across the central peak structures of four impact craters within the South Pole-Aitken Basin (SPA). Two distinct causes of spectral diversity are observed. Spectral variations across the central peaks of Bhabha, Finsen, and Lyman are dominated by soil development, including the effects of space weathering and mixing with local materials. For these craters, the central peak structure is homogeneous in composition, although small compositional differences between the craters are observed. This group of craters is located within the estimated transient cavity of SPA, and their central uplifts exhibit similar mafic abundances. Therefore, it is plausible that they have all uplifted material associated with melts of the lower crust or upper mantle produced during the SPA impact. Compositional differences observed between the peaks of these craters reflect heterogeneities in the SPA subsurface, although the origin of this heterogeneity is uncertain. In contrast to these craters, Leeuwenhoek exhibits compositional heterogeneity across its central peak structure. The peak is areally dominated by feldspathic materials, interspersed with several smaller exposures exhibiting a mafic spectral signature. Leeuwenhoek is the largest crater included in the study and is located in a region of complex stratigraphy involving both crustal (feldspathic) and SPA (mafic melt and ejecta) materials. The compositional diversity observed in Leeuwenhoek's central peak indicates that kilometer-scale heterogeneities persist to depths of more than 10 km in this region.

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A model for the thermal and chemical evolution of the Moon's interior: implications for the onset of mare volcanism

Cited by 368 publications

References 25 publications

Thermal evolution of a thicker KREEP liquid layer

Thermal evolution of a thicker KREEP liquid layer

Phase equilibria of ultramafic compositions on Mercury and the origin of the compositional dichotomy

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

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