Asteroid spectral types
Asteroids are assigned a type based on spectral shape,
color, and sometimes albedo. These types are thought to correspond to an asteroid's surface composition. For small bodies which are not internally differentiated, the surface and internal compositions are presumably similar, while large bodies such as 1 Ceresand 4 Vestaare known to have internal structure.
A list of types can be found at .
The present-day classification was initiated by Clark R. Chapman, David Morrison, and Ben Zellner in 1975 1 with three categories: C for dark carbonaceous objects, S for stony (silicaceous) objects, and U for those which did not fit into either C or S. This classification has since been expanded and clarified.
A number of classification schemes are currently in existence 23, and while they strive to retain some mutual consistency, quite a few asteroids are sorted into different classes depending on the particular scheme. This is due to the use of different criteria for each approach. The two most widely used classifications are described below:
The most widely used taxonomy for over a decade has been that of
David J. Tholen, first proposed in 1984. This classification was developed from broad band spectra (between 0.31μm and 1.06μm) obtained during the Eight-Color Asteroid Survey (ECAS) in the 1980s, in combination with albedomeasurements 4. The original formulation was based on 978 asteroids.
This scheme includes 14 types with the majority of asteroids falling into one of three broad categories, and several smaller types. They are, with their largest exemplars:
*C-group dark carbonaceous objects, including several sub-types:
10 Hygiea) the remaining majority of 'standard' C-type asteroids. This group contains about 75% of asteroids in general.
15 Eunomia, 3 Juno) silicaceous (i.e. stony) objects. This class contains about 17% of asteroids in general.
16 Psyche) metallic objects, the third most populous group.
44 Nysa, 55 Pandora) differ from M-type mostly by high albedo
259 Aletheia, 190 Ismene; CP: 324 Bamberga) differ from M-type mostly by low albedoand the small classes:
4 Vesta)Objects were sometimes assigned a combined type such as "e.g." CG when their properties were a combination of those typical for several types.
This is a more recent taxonomy introduced by Schelte J. Bus and Richard P. Binzel in 2002, based on the Small Main-Belt Asteroid Spectroscopic Survey (SMASS) of 1447 asteroids 5. This survey produced spectra of a far higher resolution than ECAS, and was able to resolve a variety of narrow spectral features. However, a somewhat smaller range of wavelengths (0.44μm to 0.92μm) was observed. Also, albedos were not considered. While attempting to keep to the Tholen taxonomy as much as possible given the differing data, asteroids were sorted into the 24 types given below. The majority of bodies fall again into the three broad C, S, and X categories, with a few unusual bodies categorized into several smaller types:
*C-group of carbonaceous objects including:
**B-type largely overlapping with the Tholen B and F types.
**C-type the most 'standard' of the non-B carbonaceous objects
**Cg Ch Cgh somewhat related to the Tholen G type
**Cb transition objects between plain C and B types.
*S-group of silicaceous (stony) objects including:
**K-type a new category (
181 Eucharis, 221 Eos)
**L-type a new category (
**S-type the most 'standard' of the S group
**Sa, Sq, Sr, Sk, and Sl transition objects between plain S and the other types in the group.
*X-group of mostly metallic objects including:
**X-type the most 'standard' of the X group including objects classified by Tholen as M, E, or P-type.
**Xe, Xc, and Xk transition types between plain X and the appropriately lettered types.
*Ld-type: a new type with more extreme spectral features than the L-type
*O-type a small category (
A significant number of small asteroids were found to fall in the Q, R, and V types, which were represented by only a single body in the Tholen scheme.In this Bus and Binzel SMASS scheme only a single type was assigned to any particular asteroid.
Near-Earth objectshave spectra which differ strongly from any of the SMASS classes. This is presumably because these bodies are much smaller than those detected in the Main Belt, and as such may have younger less-altered surfaces or be composed of a less varied mix of minerals.
These classification schemes are expected to be refined and/or replaced as further research progresses. However, for now , the spectral classification based on the two above coarse resolution spectroscopic surveys from the 1990s is still the standard. Scientists have been unable to agree on a better taxonomic system, largely due to the difficulty of obtaining detailed measurements consistently for a large sample of asteroids (e.g. finer resolution spectra, or non-spectral data such as densities would be very useful).
#C. R. Chapman, D. Morrison, and B. Zellner "Surface properties of asteroids: A synthesis of polarimetry, radiometry, and spectrophotometry", Icarus, Vol. 25, pp. 104 (1975).
#D. J. Tholen "Asteroid taxonomic classifications" in Asteroids II, pp. 1139-1150, University of Arizona Press (1989).
#S. J. Bus, F. Vilas, and M. A. Barucci "Visible-wavelength spectroscopy of asteroids" in Asteroids III, pp. 169, University of Arizona Press (2002).
#S. J. Bus and R. P. Binzel "Phase II of the Small Main-belt Asteroid Spectroscopy Survey: A feature-based taxonomy", Icarus, Vol. 158, pp. 146 (2002).
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