Spectral reflectance properties of carbonaceous chondrites: 8. “Other” carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions, and R chondrites

Cloutis, E. A.; Hudon, Pierre; Hiroi, T.; Gaffey, M. J.; Mann, P.

doi:10.1016/j.icarus.2012.10.008

Cited by 38 publications

(42 citation statements)

References 67 publications

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“…Trigo-Rodriguez et al (2006), 3 Rubin (2007), 4 Gounelle et al (2001). †When provided, wavelength region where brightening occurs is given, §A unique meteorite with affinities to CM and CI chondrites (Zolensky et al 2002;Cloutis et al 2012). NOTE.-Each of the models were produced using mean grain diameters of 37.5µm.…”

Section: Resultsmentioning

confidence: 99%

Simulated space weathering of Fe- and Mg-rich aqueously altered minerals using pulsed laser irradiation

Kaluna

Ishii

Bradley

et al. 2017

Icarus

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Simulated space weathering experiments on volatile-rich carbonaceous chondrites (CCs) have resulted in contrasting spectral behaviors (e.g. reddening vs bluing). The aim of this work is to investigate the origin of these contrasting trends by simulating space weathering on a subset of minerals found in these meteorites. We use pulsed laser irradiation to simulate micrometeorite impacts on aqueously altered minerals and observe their spectral and physical evolution as a function of irradiation time. Irradiation of the mineral lizardite, a Mg-phyllosilicate, produces a small degree of reddening and darkening, but a pronounced reduction in band depths with increasing irradiation. In comparison, irradiation of an Fe-rich aqueously altered mineral assemblage composed of cronstedtite, pyrite and siderite, produces significant darkening and band depth suppression. The spectral slopes of the Fe-rich assemblage initially redden then become bluer with increasing irradiation time. Post-irradiation analyses of the Fe-rich assemblage using scanning and transmission electron microscopy reveal the presence of micron sized carbon-rich particles that contain notable fractions of nitrogen and oxygen. Radiative transfer modeling of the Fe-rich assemblage suggests that nanometer sized metallic iron (npFe 0 ) particles result in the initial spectral reddening of the samples, but the increasing production of micron sized carbon particles (µpC) results in the subsequent spectral bluing. The presence of npFe 0 and the possible catalytic nature of cronstedtite, an Fe-rich phyllosilicate, likely promotes the synthesis of these carbon-rich, organic-like compounds. These experiments indicate that space weathering processes may enable organic synthesis reactions on the surfaces of volatile-rich asteroids. Furthermore, Mg-rich and Fe-rich aqueously altered minerals are dominant at different phases of the aqueous alteration process. Thus, the contrasting spectral slope evolution between the Fe-and Mg-rich samples in these experiments may indicate that space weathering trends of volatilerich asteroids have a compositional dependency that could be used to determine the aqueous histories of asteroid parent bodies.

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Section: Resultsmentioning

confidence: 99%

Simulated space weathering of Fe- and Mg-rich aqueously altered minerals using pulsed laser irradiation

Kaluna

Ishii

Bradley

et al. 2017

Icarus

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“…The rare olivine-dominated R-type chondrites (Rumurutites - Kallemeyn et al, 1996) show a strong olivine feature in their spectra (e.g., Berlin, 2003;Berlin et al, 2003;Sunshine et al, 2007;Cloutis et al, 2012a). Finer particle size fractions of CK chondrites also exhibit a nearly pure olivine absorption feature albeit much weaker .…”

Section: Discussionmentioning

confidence: 99%

Asteroid (354) Eleonora: Plucking an odd duck

Gaffey

Reddy

Fieber-Beyer

et al. 2015

Icarus

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a b s t r a c t During a survey of the S-type asteroids, Gaffey et al. (Gaffey, M.J., Bell, J.F., Brown, R.H., Burbine, T.H.,Piatek, J., Reed, K.L., Chaky, D.A. [1993]. Icarus 106, 573-602) identified Asteroid (354) Eleonora as anomalous with a 1 lm absorption feature $2.5 times stronger than any S-asteroid of comparable size. Subsequent investigation revealed significant differences in the 1 lm absorption feature between the visible & very near-infrared CCD spectra (k < $1.0 lm) and other spectral data sets for this asteroid. There were also significant spectral differences among the several CCD survey spectra (SMASS-I, SMASS-II & S 3 OS 2 ) of Eleonora. These differences could potentially arise from spectral variations across the asteroid surface, from observational phase angle differences, from surface temperature differences, from viewing geometry for a nonspherical body, or from the use of standard stars with deviated to different degrees from a true solar standard.In June 2011 Asteroid (354) Eleonora was observed over two nights using the NASA Infrared Telescope Facility (IRTF) at Mauna Kea Observatory in order to test these possible scenarios and to better understand the nature and history of Eleonora and its relationships to other asteroids and to the meteorites. Analysis of this data set has eliminated the following options as the cause of the differences in the 1 lm absorption feature within the CCD data sets and between the CCD data sets and the other spectral data: (1) rotational spectral variations; (2) variation in surface composition with latitude; (3) observation phase; (4) surface temperature variations with differing heliocentric distance in the asteroid's elliptical orbit; (5) spectral effects of viewing geometry for a nonspherical body; and (6) differences in spectral standard stars. We conclude that none of the CCD spectra of (354) Eleonora are reliable, and that within the limits of their spectral coverage, analyses of the three CCD spectra would produce significantly different -and generally unreliable -indications of surface mineralogy. An effort needs to be made to determine whether ''bad'' CCD spectra are rare with the case of (354) Eleonora being an uncommon occurrence or whether there is a broader problem with the CCD asteroid survey data sets, and if so, how to identify the ''bad'' spectra.While CCD survey spectra show apparently irreconcilable differences, the near-infrared spectra of (354) Eleonora from various observers show only minor differences, primarily in the overall spectral slope, most of which can be attributed to slight differences in the standard stars used to calibrate the data.In June 2011, 226 near-infrared ($0.76-2.5 lm) spectra of (354) Eleonora were obtained using the SpeX instrument on the NASA Infrared Telescope Facility at Mauna Kea Observatory. These spectra were consistent with the six sets of NIR spectra obtained for Eleonora by previous observers. The primary variation observed in this new data set was an approximately 10% variation in spectral slope between...

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“…), grain size (e.g., Cloutis et al. ; Binzel et al. ), and age of the surface regolith (e.g., Riner and Lucey ), therefore highlighting both the chemico‐physical state and space weathering processes.…”

Section: Tools and Techniquesmentioning

confidence: 99%

Mineralogy and temperature of crater Haulani on Ceres

Tosi

Carrozzo

Raponi

et al. 2018

Meteorit & Planetary Scien

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We investigate the region of crater Haulani on Ceres with an emphasis on mineralogy as inferred from data obtained by Dawn's Visible InfraRed mapping spectrometer (VIR), combined with multispectral image products from the Dawn Framing Camera (FC) so as to enable a clear correlation with specific geologic features. Haulani, which is one of the youngest craters on Ceres, exhibits a peculiar "blue" visible to nearinfrared spectral slope, and has distinct color properties as seen in multispectral composite images. In this paper, we investigate a number of spectral indices: reflectance; spectral slopes; abundance of Mg-bearing and NH 4 -bearing phyllosilicates; nature and abundance of carbonates, which are diagnostic of the overall crater mineralogy; plus a temperature map that highlights the major thermal anomaly found on Ceres. In addition, for the first time we quantify the abundances of several spectral endmembers by using VIR data obtained at the highest pixel resolution (~0.1 km). The overall picture we get from all these evidences, in particular the abundance of Na-and hydrous Na-carbonates at specific locations, confirms the young age of Haulani from a mineralogical viewpoint, and suggests that the dehydration of Na-carbonates in the anhydrous form Na 2 CO 3 may be still ongoing.

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Spectral reflectance properties of carbonaceous chondrites: 8. “Other” carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions, and R chondrites

Cited by 38 publications

References 67 publications

Simulated space weathering of Fe- and Mg-rich aqueously altered minerals using pulsed laser irradiation

Simulated space weathering of Fe- and Mg-rich aqueously altered minerals using pulsed laser irradiation

Asteroid (354) Eleonora: Plucking an odd duck

Mineralogy and temperature of crater Haulani on Ceres

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