An Oxygen Isotope Model for the Composition of Mars

Lodders, K.; Fegley, B.

doi:10.1006/icar.1996.5653

Cited by 313 publications

(368 citation statements)

References 62 publications

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“…b , Smith (2004), Smith et al (2009a). c Krasnopolsky et al (1997), Lodders and Fegley (1997), Owen et al (1977). d Krasnopolsky (2007), Smith et al (2009b).…”

Section: Water Cyclementioning

confidence: 99%

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Vandaele¹,

Moreno²,

Patel³

et al. 2018

Space Sci Rev

113

117

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The NOMAD ("Nadir and Occultation for MArs Discovery") spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the comThis paper is dedicated to the memory of M. Allen, V. Formisano, and J. McConnell. position of Mars' atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.

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“…b , Smith (2004), Smith et al (2009a). c Krasnopolsky et al (1997), Lodders and Fegley (1997), Owen et al (1977). d Krasnopolsky (2007), Smith et al (2009b).…”

Section: Water Cyclementioning

confidence: 99%

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Vandaele¹,

Moreno²,

Patel³

et al. 2018

Space Sci Rev

113

117

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“…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%

“…[24] Even if the crust was hydrothermally cooled, the compositional model by Lodders and Fegley [1997] requires crustal thicknesses of less than 50 km and initial upper mantle temperatures of less than 1800 K to be compatible with the absence of lower crustal flow. Better constraints on the Martian crustal thickness could therefore potentially rule out this model and these may be obtained from the seismological experiment envisaged for the upcoming ExoMars mission.…”

Section: Discussionmentioning

confidence: 99%

“…for some compositional models of Mars are summarized in Table 1 and chondritic concentrations are given as a reference. Note, that the model by Lodders and Fegley [1997] produces twice as much heat as other compositional models.…”

Section: Thermal Modelmentioning

confidence: 99%

“…Different models for the abundances of K, Th and U have been derived from elemental analysis of the SNC meteorites [e.g., Wänke and Dreibus, 1994;Lodders and Fegley, 1997], but so far no consensus on the concentration of radioactive nuclides in the Martian interior has been reached. The heat generated by the different models proposed so far varies by more than a factor of two and is one of the major unknowns connected to the Martian thermal evolution.…”

Section: Introductionmentioning

confidence: 99%

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

Grott

Breuer

2008

Geophysical Research Letters

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[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,

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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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An Oxygen Isotope Model for the Composition of Mars

Cited by 313 publications

References 62 publications

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

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

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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