1. Department of Geological Sciences, University of Tennessee, Knoxville, Tennessee 37996, USA

Correspondence to: Michael B. Wyatt Correspondence and requests for materials should be addressed to H.Y.M. (e-mail: Email: mcsween@utk.edu).

Abstract

Mineral abundances derived from the analysis of remotely sensed thermal emission data from Mars have been interpreted to indicate that the surface is composed of basalt (Surface Type 1) and andesite (Surface Type 2)¹. The global distribution of these rock types is divided roughly along the planetary dichotomy which separates ancient, heavily cratered crust in the southern hemisphere (basalt) from younger lowland plains in the north (andesite)¹. But the existence of such a large volume of andesite is difficult to reconcile with our present understanding of the geological evolution of Mars. Here we reinterpret martian surface rock lithologies using mineral abundances from previous work¹ and new mineralogies derived from a spectral end-member set representing minerals common in unaltered and low-temperature aqueously altered basalts. Our results continue to indicate the dominance of unaltered basalt in the southern highlands, but reveal that the northern lowlands can be interpreted as weathered basalt as an alternative to andesite. The coincidence between locations of such altered basalt and a suggested northern ocean basin implies that lowland plains material may be composed of basalts weathered under submarine conditions or weathered basaltic sediments transported into this depocentre.

1. Department of Geological Sciences, University of Tennessee, Knoxville, Tennessee 37996, USA

Correspondence to: Michael B. Wyatt Correspondence and requests for materials should be addressed to H.Y.M. (e-mail: Email: mcsween@utk.edu).