Asteroid Modal Mineralogy Using Hapke Mixing Models: Validation with HED Meteorites

The mineralogical characterization of asteroid surfaces is accomplished through the interpretation of terrestrial or space-based visible/near-infrared reflectance (VNIR) spectroscopy. This is the most sensitive technique for asteroid remote sensing and has been widely used to estimate the surface mineralogy for many asteroids. The spectral properties of asteroid surfaces are governed by the properties of the asteroid regolith, including the mineralogy, physical properties, the amount of impact-produced glass, and the degree of space weathering. Hapke s formulations [1,2,] and the recent work of [3] has permitted the creation and utilization of a model designed to produce a simulated spectrum of a given asteroid surface given a modal mineralogy, within simplifying assumptions. In [4], Clark and coworkers employed this model to make determinations about the composition and degree of space weathering on the bright and dark regions in and adjacent to Pysche crater on asteroid 433 Eros. Here, we share results of our efforts to validate the model using published mineral modes and spectra from eucrites and diogenites.