Core formation in the Earth and Shergottite Parent Body (SPB): Chemical evidence from basalts

Treiman, Allan H.; Drake, M. J.; Janssens, Marie-Josée; Wolf, Rudolf; Ebihara, Mitsuru

doi:10.1016/0016-7037(86)90389-3

Cited by 128 publications

(120 citation statements)

References 38 publications

Supporting

Mentioning

113

Contrasting

Order By: Relevance

“…Second, geochemical analysis of the SNC meteorites implies essentially chondritic concentrations of radioactive elements (Wänke and Dreibus, 1994;Treiman et al, 1986;Lodders and Fegley, 1997). Furthermore, if the concentration of heat producing elements in the Martian interior is indeed reduced, the resulting low interior temperatures could possibly inhibit partial mantle melting and magmatism.…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

“…Different models for the bulk composition of Mars have been proposed (Morgan and Anders, 1979;Treiman et al, 1986;Wänke and Dreibus, 1994;Lodders and Fegley, 1997), but it seems unlikely that compositional models which generate heat at rates larger than the chondritic heat production rate (e.g., Lodders and Fegley (1997)) are representative of the planet's bulk composition (Hauck and Phillips, 2002;Grott and Breuer, 2008b). The model by Wänke and Dreibus (1994) is the one best compatible with the amount of K and Th in the near surface layers as observed by gamma ray spectroscopy (Taylor et al, 2006) and we will use this model as a reference.…”

Section: Parametersmentioning

confidence: 99%

See 1 more Smart Citation

Implications of large elastic thicknesses for the composition and current thermal state of Mars

Grott

Breuer

2009

Icarus

View full text Add to dashboard Cite

To cite this version:M. Grott, D. Breuer. Implications of large elastic thicknesses for the composition and current thermal state of Mars. Icarus, Elsevier, 2009, 201 (2) This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. A C C E P T E D M A N U S C R I P T ACCEPTED MANUSCRIPT A C C E P T E D M A N U S C R I P T ACCEPTED MANUSCRIPT AbstractThe Martian elastic lithosphere thickness T e has recently been constrained by modeling the geodynamical response to loading at the Martian polar caps and T e was found to exceed 300 km at the north pole today. Geological evidence suggests that Mars has been volcanically active in the recent past and we have reinvestigated the Martian thermal evolution, identifying models which are consistent with T e > 300 km and the observed recent magmatic activity. We find that although models satisfying both constraints can be constructed, special assumptions regarding the concentration and distribution of radioactive elements, the style of mantle convection and/or the mantle's volatile content need to be made. If a dry mantle rheology is assumed, strong plumes caused by, e.g., a strongly pressure dependent mantle viscosity or endothermic phase transitions near the core-mantle boundary are required to allow for decompression melting in the heads of mantle plumes. For a wet mantle, large mantle water contents of the order of 1000 ppm are required to allow for partial mantle melting. Also, for a moderate crustal enrichment of heat producing, elements the planet's bulk composition needs to be 25% and 50% sub-chondritic for dry and wet mantle rheologies, respectively. Even then, models resulting in a globally averaged elastic thicknesses of T e > 300 km are difficult to reconcile with most elastic thickness estimates available for the Hesperian and Amazonian periods. It therefore seems likely that large elastic thicknesses in excess of 300 km are not representative for the bulk of the planet and that T e possibly shows a large degree of spatial heterogeneity.

show abstract

Section: Accepted M Manuscriptmentioning

confidence: 99%

Section: Parametersmentioning

confidence: 99%

Implications of large elastic thicknesses for the composition and current thermal state of Mars

Grott

Breuer

2009

Icarus

View full text Add to dashboard Cite

show abstract

“…F) TiO 2 vs. MgO. Data are from Anand et al (2008), Dreibus et al (2000Dreibus et al ( , 2002, Gellert et al (2006), Gillet et al (2005), Ikeda et al (2006), Jambon et al (2002), , Neal et al (2001), Rubin et al (2000), Shirai and Ebihara (2004), Taylor et al (2002), Treiman et al (1986), Warren et al (1996Warren et al ( , 1999. .…”

Section: Introductionmentioning

confidence: 98%

“…Most shergottites tend to be depleted in incompatible elements, particularly in alkalis ( Fig. 1D) and light rare earth elements (REE; e.g., Treiman et al, 1986) and are likely derived from a mantle that has been depleted in these elements for a long time based on Sm-Nd isotope systematics (Harper et al, 1995;Borg et al, 1997). A second, more enriched reservoir must also exist because some shergottites have flatter REE profiles (higher La/Lu ratios) and Sm-Nd systematics that indicate prolonged incompatible element enrichment.…”

Section: Introductionmentioning

confidence: 99%

The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites

Schmidt

McCoy

2010

Earth and Planetary Science Letters

View full text Add to dashboard Cite

“…Radioactive elements in concentrations derived by Morgan and Anders [1979], Treiman et al [1986] and Wänke and Dreibus [1994] generate heat at rates smaller than 25 pW kg À1 at 4.5 Gyr b.p., consistent with the upper bounds on radiogenic heating derived here. The model by Lodders and Fegley [1997] predicts radiogenic heating at a rate of $49 pW kg À1 and is therefore incompatible with the absence of large scale topographic relaxation if no hydrothermal cooling of the crust occurred.…”

Section: Discussionmentioning

confidence: 99%

Constraints on the radiogenic heat production rate in the Martian interior from viscous relaxation of crustal thickness variations

Grott

Breuer

2008

Geophysical Research Letters

View full text Add to dashboard Cite

[1] Crustal thickness variations induce lateral pressure gradients which can drive flow in the lower crust if temperatures there are sufficiently high. The absence of large scale crustal relaxation at the Argyre impact basin therefore constrains the temperatures at the base of the crust and we have computed thermal evolution models to study the influence of radiogenic heating and hydrothermal crustal cooling on lower crustal temperatures. In the presence and absence of hydrothermal crustal cooling and for an average crustal thickness of 45 km, radiogenic heating after core formation cannot have exceeded 58 and 43 pW kg À1 , respectively. Furthermore, if the average crustal thickness is closer to 50 km, heating cannot have exceeded 49 and 36 pW kg À1 . A better knowledge of the planet's average crustal thickness, which may be obtained from seismological experiments, could help to further constrain the planets bulk composition and even rule out some of the compositional models for Mars that have been proposed so far.Citation: Grott, M., and D. Breuer (2008), Constraints on the radiogenic heat production rate in the Martian interior from viscous relaxation of crustal thickness variations, Geophys. Res. Lett., 35, L05201,

show abstract

Core formation in the Earth and Shergottite Parent Body (SPB): Chemical evidence from basalts

Cited by 128 publications

References 38 publications

Implications of large elastic thicknesses for the composition and current thermal state of Mars

Implications of large elastic thicknesses for the composition and current thermal state of Mars

The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites

Constraints on the radiogenic heat production rate in the Martian interior from viscous relaxation of crustal thickness variations

Contact Info

Product

Resources

About