Spectral characteristics of rocks: Effects of composition and texture and implications for the interpretation of planet surface compositions

In spectroscopic remote sensing for the exploration of the surface compositions of Earth and terrestrial planets, reflectance spectra with very low spectral contrast and even devoid of diagnostic absorption bands can be observed, which make the interpretation of the component minerals ambiguous. Using selected examples of terrestrial rock samples from intrusive and effusive geologic systems, we discuss compositional and textural properties related to these particular spectral shapes. We show that: (1) this spectral behaviour is common for coarse grains of multimineral rocks, where the optical coupling is expected to occur between welded mineral particles; (2) it is emphasised by the presence of opaque minerals with various compositions, such as ulvospinel, magnetite and chromite in effusive rock groundmass and in intrusive rocks; (3) it is controlled by the number of silicate phases within which the FeO is distributed, irrespective of the total iron content in the rock: a rock composition with a high number of iron-bearing minerals producing this kind of low contrast, almost featureless spectra is indicated here as “critical mode”; (4) it is also strongly intensified by aqueous alteration of silicates. observations suggest unpredictable combinations of several different petrographic variables affecting the spectra of some compact rocks, and stimulate both targeted studies to quantitatively relate spectral and petrographic parameters, and the development of appropriate methods of spectral decomposition. Our ongoing work is at present focused on the spectroscopic effects of the FeO concentration in transparent neutral plagioclase, the different compositions of the opaque neutral minerals, and the iron bearing amorphous phases. o discuss the analogy between the rocks used in the analysis reported here and the crustal rock compositions observed on Mars and inferred for Mercury as well as the compatibility of the factors responsible for the low spectral contrast of terrestrial rock samples with the factors expected for the two planets. We observe that a coarse-grained surface and a composition approaching a critical mode could explain the featureless Acidalia spectra on Mars, and suggest that the still open questions about Mercury’s surface regolith characteristics and composition do not exclude a priori the contribution of some of the factors examined in this paper to the peculiar surface properties of this planet.