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Forging asteroid-meteorite relationships through reflectance spectroscopy

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dc.contributor.advisor Richard P. Binzel. en_US
dc.contributor.author Burbine, Thomas H. (Thomas Hewey), 1966- en_US
dc.contributor.other Massachusetts Institute of Technology. Dept. of Earth, Atmospheric, and Planetary Sciences. en_US
dc.date.accessioned 2005-08-22T23:15:35Z
dc.date.available 2005-08-22T23:15:35Z
dc.date.copyright 2000 en_US
dc.date.issued 2000 en_US
dc.identifier.uri http://hdl.handle.net/1721.1/9170
dc.description Thesis (Ph.D.)--Massachusetts Institute of Technology, Dept. of Earth, Atmospheric, and Planetary Sciences, 2000. en_US
dc.description Includes bibliographical references (p. 225-248). en_US
dc.description.abstract Near-infrared spectra (~0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. These asteroids appear almost certainly to be fragments of Vesta. Spectral variations between these objects are consistent with being primarily due to differences in particle size. These asteroids also tend to have stronger band depths with increasing ejection velocity from Vesta. Objects with distinctive olivine bands appear to provide definitive evidence that spectral alteration is occurring in the asteroid belt. These objects have similar band depths but appear significantly reddened relative to measured olivine samples due to their significantly higher reflectance values with increasing wavelength. The only laboratory-simulated "weathering" process that reddens the spectra but does not significantly suppress the bands is alteration by laser irradiation, which is hoped to duplicate the effects of micrometeorite bombardment. A number of plausible main-belt parent bodies were identified. These include 19 Fortuna and the CM chondrites, Eos family members with the CO chondrites and 599 Luisa with the CV chondrites. A significant fraction of S asteroids have spectral properties that range from similar to ordinary chondrites to much redder with weaker absorption bands. These objects tend to have spectra consistent with a mixture of ordinary chondrite material and metallic iron. However, other alteration processes cannot be ruled out. Asteroids with distinctive olivine bands are relatively rare. The available evidence is consistent with a scenario where, with the exception of Vesta, all differentiated bodies were either disrupted or had their mantles stripped very early in the age of the solar system. Olivine-rich metal-free fragments were then continually broken down until they almost all now fall below our current astronomical measurement limits. en_US
dc.description.statementofresponsibility by Thomas H. Burbine, Jr. en_US
dc.format.extent 301 p. en_US
dc.format.extent 21622675 bytes
dc.format.extent 21622433 bytes
dc.format.mimetype application/pdf
dc.format.mimetype application/pdf
dc.language.iso eng en_US
dc.publisher Massachusetts Institute of Technology en_US
dc.rights M.I.T. theses are protected by copyright. They may be viewed from this source for any purpose, but reproduction or distribution in any format is prohibited without written permission. See provided URL for inquiries about permission. en_US
dc.rights.uri http://dspace.mit.edu/handle/1721.1/7582
dc.subject Earth, Atmospheric, and Planetary Sciences. en_US
dc.title Forging asteroid-meteorite relationships through reflectance spectroscopy en_US
dc.type Thesis en_US
dc.description.degree Ph.D. en_US
dc.contributor.department Massachusetts Institute of Technology. Dept. of Earth, Atmospheric, and Planetary Sciences. en_US
dc.identifier.oclc 45426609 en_US


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