Surface Material Analysis of S-type Asteroids: Removing the Space Weathering Effect from Reflectance Spectrum

Introduction: Recent years, many researchers have been observing a lot of asteroid reflectance spectra in the UV, visible to NIR at wavelength region [e.g., 1-4]. Reflectance spectroscopy of asteroid at this range should bring us a lot of information about its surface materials. Pyroxene and olivine have characteristic absorption bands in this wavelength range. Low-Ca pyroxene has two absorption bands around 0.9 μm and 1.9 μm. The more Ca and Fe content, the longer both absorption band centers. On the other hand, reflectance spectrum of olivine has three complicated absorption bands around 1 μm, and no absorption feature around 2 μm [5]. In general, reflectance spectra of many asteroids that are considered to be silicate rich (i.e., Sand Atype asteroids) show redder slope and more subdued absorption bands than those of terrestrial minerals and meteorites. These features are now believed to be caused by the space weathering effect [e.g., 6, 7], which is probably caused by micrometeorite bombardment and/or solar wind. This process causes nanophase reduced iron (npFe 0 ) particles near the surface of mineral grains, which leads the optical change. Therefore, the space weathering effect should be removed from asteroid reflectance spectra to compare with those of meteorite and terrestrial minerals. In this report, we will apply the expanded modified Gaussian model (MGM) [8] to the reflectance spectra of S-type asteroids 7 Iris and 532 Herculina and compare them with those of meteorites.