Correction to “Viscous and impact demagnetization of Martian crust”

Thermal demagnetization of Martian upper crust by magma intrusion

[1] The absent or weak magnetic field above large Martian volcanoes may provide constraints on their formation and the carrier of magnetization. We consider the ability of magma intrusions to thermally demagnetize the shallow crust beneath volcanoes through heat conduction and hydrothermal circulation. If magnetization is dominated by magnetite, the volume of crust that is thermally demagnetize...

Elemental composition of the Martian crust.

The composition of Mars' crust records the planet's integrated geologic history and provides clues to its differentiation. Spacecraft and meteorite data now provide a global view of the chemistry of the igneous crust that can be used to assess this history. Surface rocks on Mars are dominantly tholeiitic basalts formed by extensive partial melting and are not highly weathered. Siliceous or calc...

Constraints on the composition and petrogenesis of the Martian crust

[1] Spectral interpretation that silicic rocks are widespread on Mars implies that Earth’s differentiated crust is not unique. Evaluation of observations bearing on the composition of the Martian crust (Martian meteorite petrology and a possible crustal assimilant, analysis of Mars Pathfinder rocks, composition of Martian fines, interpretation of spacecraft thermal emission spectra, and inferre...

Chemical and Isotopic Constraints for the Martian Crust

Introduction: The Martian meteorite whole rock Rb-Sr isotopic compositions and the initial Pb data from plagioclase separates suggest strongly that the crust of their parent body originated from an ancient planetary global differentiation process about 4.5 Ga ago. The absence of plate tectonic activity on early Mars excludes a crustal recycling and preserves the isotopic systems derived from th...

Martian Impact Cratering and Martian Layered Sediments