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• W2786498655 abstract "Carbonaceous chondrites (CCs) are important materials for understanding the early evolution of the solar system and delivery of volatiles and organic material to the early Earth. Presumed CC-like asteroids are also the targets of two current sample return missions: OSIRIS-REx to asteroid Bennu and Hayabusa-2 to asteroid Ryugu, and the Dawn orbital mission at asteroid Ceres. To improve our ability to identify and characterize CM2 CC-type parent bodies, we have examined how factors such as particle size, particle packing, and viewing geometry affect reflectance spectra of the Murchison CM2 CC. The derived relationships have implications for disc-resolved examinations of dark asteroids and sampleability. It has been found that reflectance spectra of slabs are more blue-sloped (reflectance decreasing toward longer wavelengths as measured by the 1.8/0.6 µm reflectance ratio), and generally darker, than powdered sample spectra. Decreasing the maximum grain size of a powdered sample results in progressively brighter and more red-sloped spectra. Decreasing the average grain size of a powdered sample results in a decrease in diagnostic absorption band depths, and redder and brighter spectra. Decreasing porosity of powders and variations in surface texture result in spectral changes that may be different as a function of viewing geometry. Increasing thickness of loose dust on a denser powdered substrate leads to a decrease in absorption band depths. Changes in viewing geometry lead to different changes in spectral metrics depending on whether the spectra are acquired in backscatter or forward-scatter geometries. In backscattered geometry, increasing phase angle leads to an initial increase and then decrease in spectral slope, and a general decrease in visible region reflectance and absorption band depths, and frequent decreases in absorption band minima positions. In forward scattering geometry, increasing phase angle leads to small non-systematic changes in spectral slope, and general decreases in visible region reflectance, and absorption band depths. The highest albedos and larger band depths are generally seen in the lowest phase angle backscattering geometry spectra. The reddest spectra are generally seen in the lowest phase angle backscatter geometry spectra. For the same phase angle, spectra acquired in forward scatter geometry are generally redder and darker and have shallower absorption bands than those acquired in backscatter geometry. Overall, backscatter geometry-acquired spectra are flatter, brighter, and have deeper 0.7 µm region absorption band depths than forward scatter geometry-acquired spectra. It was also found that the 0.7, 0.9, and 1.1 µm absorption bands in Murchison spectra, which are attributable to various Fe electronic processes, are ubiquitous and can be used to recognize CM2 chondrites regardless of the physical properties of the meteorite and viewing geometry." @default.
• W2786498655 created "2018-02-23" @default.
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• W2786498655 date "2018-05-01" @default.
• W2786498655 modified "2023-10-11" @default.
• W2786498655 title "Spectral reflectance “deconstruction” of the Murchison CM2 carbonaceous chondrite and implications for spectroscopic investigations of dark asteroids" @default.
• W2786498655 cites W1969380539 @default.
• W2786498655 cites W1970117818 @default.
• W2786498655 cites W1974511717 @default.
• W2786498655 cites W1974923710 @default.
• W2786498655 cites W1976015855 @default.
• W2786498655 cites W1977071564 @default.
• W2786498655 cites W1977176399 @default.
• W2786498655 cites W1977287712 @default.
• W2786498655 cites W1978675181 @default.
• W2786498655 cites W1979727587 @default.
• W2786498655 cites W1982486756 @default.
• W2786498655 cites W1983013782 @default.
• W2786498655 cites W1986530877 @default.
• W2786498655 cites W1992682948 @default.
• W2786498655 cites W1994842341 @default.
• W2786498655 cites W1999941583 @default.
• W2786498655 cites W2001304874 @default.
• W2786498655 cites W2008326452 @default.
• W2786498655 cites W2009808002 @default.
• W2786498655 cites W2017998168 @default.
• W2786498655 cites W2019038438 @default.
• W2786498655 cites W2019156753 @default.
• W2786498655 cites W2019706429 @default.
• W2786498655 cites W2023688816 @default.
• W2786498655 cites W2028581564 @default.
• W2786498655 cites W2031569881 @default.
• W2786498655 cites W2032621232 @default.
• W2786498655 cites W2035388653 @default.
• W2786498655 cites W2041291817 @default.
• W2786498655 cites W2042857566 @default.
• W2786498655 cites W2043597651 @default.
• W2786498655 cites W2045424355 @default.
• W2786498655 cites W2046270819 @default.
• W2786498655 cites W2048501220 @default.
• W2786498655 cites W2048870280 @default.
• W2786498655 cites W2049486649 @default.
• W2786498655 cites W2051374087 @default.
• W2786498655 cites W2054780676 @default.
• W2786498655 cites W2055270488 @default.
• W2786498655 cites W2055619106 @default.
• W2786498655 cites W2057653709 @default.
• W2786498655 cites W2057737559 @default.
• W2786498655 cites W2059461957 @default.
• W2786498655 cites W2063021893 @default.
• W2786498655 cites W2064901860 @default.
• W2786498655 cites W2065423263 @default.
• W2786498655 cites W2075380887 @default.
• W2786498655 cites W2078016728 @default.
• W2786498655 cites W2079700249 @default.
• W2786498655 cites W2081231077 @default.
• W2786498655 cites W2085879809 @default.
• W2786498655 cites W2087930533 @default.
• W2786498655 cites W2092362339 @default.
• W2786498655 cites W2093411061 @default.
• W2786498655 cites W2094235109 @default.
• W2786498655 cites W2096282597 @default.
• W2786498655 cites W2104186868 @default.
• W2786498655 cites W2106526700 @default.
• W2786498655 cites W2111661335 @default.
• W2786498655 cites W2116147979 @default.
• W2786498655 cites W2118716221 @default.
• W2786498655 cites W2134174728 @default.
• W2786498655 cites W2154022067 @default.
• W2786498655 cites W2192394225 @default.
• W2786498655 cites W2198116561 @default.
• W2786498655 cites W2400767180 @default.
• W2786498655 cites W2513818801 @default.
• W2786498655 cites W2580184229 @default.
• W2786498655 cites W2759940313 @default.
• W2786498655 cites W2951193786 @default.
• W2786498655 cites W4211021246 @default.
• W2786498655 cites W4211069103 @default.
• W2786498655 cites W4246069094 @default.
• W2786498655 doi "https://doi.org/10.1016/j.icarus.2018.01.015" @default.
• W2786498655 hasPublicationYear "2018" @default.
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