Needless to say, near-shoemaker's results for Eros represent only a single asteroid within the improve very large and heterogeneous S-type class and cannot be blithely applied to all other S-types. . However, Eros represents a particularly pertinent test of the inferences previously made from groundbased studies. . On the one hand, the mean groundbased reflectance spectrum of Eros appears to be in the S(IV) subclass of Gaffey. (1993 thought at the time to be more likely (or least unlikely) to be oc's than any other S-type subclass. . On the other hand, reinterpretation of groundbased spectra of Eros by murchie pieters (1996) revealed possible hemispheric variations that were considerably greater than would be expected for a homogeneous, non-differentiated parent body (i.e. Outside of the bounds of such known variations within one type of oc as the range of petrologic class). Partway through near-shoemaker's orbital mission, it has become fairly clear what the final picture of Eros' mineralogy will. . Its evident spatial homogeneity in spectral properties, as observed by both the near-Infrared Spectrometer (NIS) and especially by the multispectral Imager (msi as well as preliminary chemical data from the x-ray detector (thanks to energetic solar flares accompanying solar maximum) both point away from any.
Abundant evidence assembled in the last five years has swung the pendulum strongly in favor of the second option - that some or many s-types are space-weathered oc's - including analysis of spatial variations in the reflectance spectrum of Ida (Chapman, 1996 analysis of the. nevertheless, the arguments have been indirect and remain debatable. The near-shoemaker mission to Eros has provided the first opportunity to take the analysis of an S-type's composition to the next level. . near-shoemaker's complement of instruments was designed to measure an independent suite of remotely sensed indicators of mineralogical and chemical composition with sufficient precision to distinguish between the major meteorite types. . The measurement techniques are x-ray, γ-ray, near-ir spectroscopy, and multi-spectral imaging, in addition to constraints provided for bulk density from the radio science, laser-ranging, and imaging experiments. . In addition, near-shoemaker was planned to achieve unprecedented spatial resolution for multispectral imaging and near-ir spectroscopy by orbiting Eros at much closer distances than were reached by the distant Galileo flybys of the s-type asteroids Gaspra and Ida. . Compositional variations across the surface of an asteroid can be especially diagnostic, as first demonstrated by gaffey (1984) from spectral differences resolved only hemispherically; Chapman (1996) later studied compositional variations on Ida at Galileo's much higher resolution.
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The latter have been ascribed to recent, fresh units (impact penetration to bedrock and irregular distribution of fresh ejecta around Ida) which contrast with the redder coloration of most of Ida's surface, explained by an as-yet-unidentified "space weathering" process that reddens Ida's surface with time. . Eros exhibits the same reddened coloration as Ida, presumably due to space-weathering inasmuch as near's X-ray compositional measurements indicate that Eros has an l- or ll-chondrite-like composition which should not appear to be so red. . Here we attribute the lack of any fresh units having ordinary chondrite-like colors to a plausible 50 Myr hiatus in cratering of Eros following its dynamical removal from the impact environment of the main asteroid belt, during which space weathering has reached maturity everywhere. Other possible implications of such a cratering hiatus are also discussed, including implications for the origin of the numerous boulders on Eros and the possible role of usually minor geological processes in shaping the geomorphology of Eros. Introduction, some fundamental issues in planetary science depend on identifying meteorite parent bodies. .
There has been a wide presumption that ordinary chondritic and carbonaceous chondritic material represents the predominant material in the inner solar system at the time of planetary accretion. . In addition, the differentiated meteorites dissertation show that an uncertain fraction of primordial material was heated to the point of melting at early times. . so it remains uncertain whether non-differentiated chondritic material (as represented in our meteorite collections) is representative of the materials from which the planets accreted. One of the longest standing issues in asteroid science has been the nature of S-type asteroids, the second most common type of asteroid, and their relationship to meteorites. . In particular, there has been debate about whether (a) meteorites are a highly selective, non-representative sample of inner-main-belt asteroids and that the apparent spectral dissimilarity between S-types and the common ordinary chondrites (OC's) means that the common S-type asteroids are parents of rare or non-sampled.
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