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 that are not internally differentiated, the surface and internal compositions are presumably similar, while large bodies such as 1 Ceres and 4 Vesta are known to have internal structure.
A list of types can be found at asteroid spectral classes.
The present-day classification was initiated by Clark R. Chapman, David Morrison, and Ben Zellner in 1975 with three categories: C for dark carbonaceous objects, S for stony (silicaceous) objects, and U for those that 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, 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 0.31 μm and 1.06 μm) obtained during the Eight-Color Asteroid Survey (ECAS) in the 1980s, in combination with albedo measurements. 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.
- S-type (15 Eunomia, 3 Juno) silicaceous (or "stony") objects.
and the small classes:
- A-type (246 Asporina)
- D-type (624 Hektor)
- T-type (96 Aegle)
- Q-type (1862 Apollo)
- R-type (349 Dembowska)
- V-type (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 1,447 asteroids. 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 (0.44 μm to 0.92 μm) was observed. Also, albedos were not considered. 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:
- S-group of silicaceous (stony) objects including:
- 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 (3628 Božněmcová)
- V-type (4 Vesta)
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.
A few near-Earth objects have spectra that differ strongly from any of the SMASS classes. This is presumably because these bodies are much smaller than those detected in the asteroid belt, and as such may have younger less-altered surfaces or be composed of a less varied mix of minerals.
In the a photometric system, the brightness of an object can be measured through a set of different, wavelength-specific filters (passbands). In the UBV photometric system, three different filters are used:
- U: passband for the ultraviolet light
- B: passband for the blue light
- V: passband sensitive to visible light, more specifically the green-yellow portion of the visible light
In an observation, the brightness of an object is measured twice through a different filter. The resulting difference in magnitude is called the color index. The U–B or B–V color indices are the most common ones.
|Wavelengths||380–450 nm||450–495 nm||495–570 nm||570–590 nm||590–620 nm||620–750 nm|
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).
Some groupings of asteroids have been correlated with meteorite types:
- C-type - Carbonaceous chondrite meteorites
- S-type - Stony meteorites
- M-type - Iron meteorites
- V-type - HED meteorites
- Chapman, C. R.; Morrison, D.; Zellner, B. (1975). "Surface properties of asteroids: A synthesis of polarimetry, radiometry, and spectrophotometry". Icarus 25 (1): 104–130. Bibcode:1975Icar...25..104C. doi:10.1016/0019-1035(75)90191-8.
- Bus, S. J.; Vilas, F.; Barucci, M. A. (2002). "Visible-wavelength spectroscopy of asteroids". Asteroids III. Tucson: University of Arizona Press. p. 169. ISBN 0-8165-2281-2.
- Tholen, D. J. (1989). "Asteroid taxonomic classifications". Asteroids II. Tucson: University of Arizona Press. pp. 1139–1150. ISBN 0-8165-1123-3.
- Bus, S. J.; Binzel, R. P. (2002). "Phase II of the Small Main-belt Asteroid Spectroscopy Survey: A feature-based taxonomy". Icarus 158 (1): 146–177. Bibcode:2002Icar..158..146B. doi:10.1006/icar.2002.6856.