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1
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42549152647
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CAIs have been dated using lead isotopes at 4.566 billion years ago (+2 million years ago/-1 million years ago) by Allègre et al. (36) and 4.5647 (±0.0006) billion years ago by Amelin et al. (37).
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CAIs have been dated using lead isotopes at 4.566 billion years ago (+2 million years ago/-1 million years ago) by Allègre et al. (36) and 4.5647 (±0.0006) billion years ago by Amelin et al. (37).
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2
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0000338356
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J. J. Papike, Ed, Mineralogic Society of America, Washington, DC
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A. J. Brearley, R. H. Jones, in Reviews In Mineralogy, Vol. 36, Planetary Materials, J. J. Papike, Ed. (Mineralogic Society of America, Washington, DC, 1998), pp. 3-1-3-398.
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(1998)
Reviews In Mineralogy, Vol. 36, Planetary Materials
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Brearley, A.J.1
Jones, R.H.2
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4
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42549122387
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Other common Fe-bearing silicates that have strong absorptions in the near infrared (38). Although pyroxene spectra have absorptions in the 2-μm region, they have even stronger features near 1 μm. Conversely, olivine spectra lack 2-μm absorptions and are instead characterized by a complex feature at 1 μm. It is on this basis (a strong 2-μm absorption in the absence of a stronger 1-μm feature) that spinel is spectrally identified.
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Other common Fe-bearing silicates that have strong absorptions in the near infrared (38). Although pyroxene spectra have absorptions in the 2-μm region, they have even stronger features near 1 μm. Conversely, olivine spectra lack 2-μm absorptions and are instead characterized by a complex feature at 1 μm. It is on this basis (a strong 2-μm absorption in the absence of a stronger 1-μm feature) that spinel is spectrally identified.
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5
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42549129022
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This nomenclature was primarily designed for use in classifying CAIs from CV3 meteorites. Over the last three decades other descriptive terminology has been developed for other chondrite types 9, 39
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This nomenclature was primarily designed for use in classifying CAIs from CV3 meteorites. Over the last three decades other descriptive terminology has been developed for other chondrite types (9, 39).
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6
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42549086061
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H. C. Connolly Jr., S. J. Desch, R. D. Ash, R. H. Jones, in Meteorites and the Early Solar System II, D. S. Lauretta, H. Y. McSween Jr., Eds. (Univ. of Arizona Press, Tucson, AZ, 2006), pp. 383-397.
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H. C. Connolly Jr., S. J. Desch, R. D. Ash, R. H. Jones, in Meteorites and the Early Solar System II, D. S. Lauretta, H. Y. McSween Jr., Eds. (Univ. of Arizona Press, Tucson, AZ, 2006), pp. 383-397.
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7
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33845685808
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M. E. Zolensky et al., Science 314, 1735 (2006).
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(2006)
Science
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Zolensky, M.E.1
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9
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0024225161
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J. F. Kerridge, M. S. Matthews, Eds, Univ. of Arizona Press, Tucson, AZ
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G. J. MacPherson, D. A. Wark, J. T. Armstrong, in Meteorites and the Early Solar System, J. F. Kerridge, M. S. Matthews, Eds. (Univ. of Arizona Press, Tucson, AZ, 1988), pp. 746-807.
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, pp. 746-807
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MacPherson, G.J.1
Wark, D.A.2
Armstrong, J.T.3
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10
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42549111956
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The Smithsonian Allende sample USNM 3509 was sectioned into large slices, and refractory inclusions were identified and cored. Thin and thick sections were made from half of the objects, and reference materials were preserved for future study. Thin sections were analyzed by the Cameca SX50 electron microprobe at the Lunar and Planetary Laboratory at the University of Arizona to quantify major and minor element abundances. While avoiding contamination from the matrix, material from the other half of the objects was cored out, ground into <38-μm-size powders, and sent to Brown University for spectral measurements at the NASA-Keck Reflectance Experiment Laboratory (RELAB) facility 40, All spectra were measured with 5-nm resolution at a standard viewing geometry of 30° incidence, 0° emission
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The Smithsonian Allende sample USNM 3509 was sectioned into large slices, and refractory inclusions were identified and cored. Thin and thick sections were made from half of the objects, and reference materials were preserved for future study. Thin sections were analyzed by the Cameca SX50 electron microprobe at the Lunar and Planetary Laboratory at the University of Arizona to quantify major and minor element abundances. While avoiding contamination from the matrix, material from the other half of the objects was cored out, ground into <38-μm-size powders, and sent to Brown University for spectral measurements at the NASA-Keck Reflectance Experiment Laboratory (RELAB) facility (40). All spectra were measured with 5-nm resolution at a standard viewing geometry of 30° incidence, 0° emission.
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11
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2342513099
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S. Xu, R. P. Binzel, T. H. Burbine, S. J. Bus, Icarus 115, 1 (1995).
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S. Xu, R. P. Binzel, T. H. Burbine, S. J. Bus, Icarus 115, 1 (1995).
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13
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10444226526
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J. T. Rayner, P. M. Onaka, M. C. Cushing, C. Michael, W. D. Vacca, Proc. SPIE 5492, 1498 (2004).
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(2004)
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Rayner, J.T.1
Onaka, P.M.2
Cushing, M.C.3
Michael, C.4
Vacca, W.D.5
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14
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42549133364
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In the Bus visible asteroid taxonomy, objects with a steep red spectral slope at wavelengths up to 0.75 μm, which are then relatively flat, are classified as L types 41
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In the Bus visible asteroid taxonomy, objects with a steep red spectral slope at wavelengths up to 0.75 μm, which are then relatively flat, are classified as L types (41).
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15
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42549105309
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S. J. Bus, thesis, Massachusetts Institute of Technology, (1999).
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S. J. Bus, thesis, Massachusetts Institute of Technology, (1999).
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16
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0000284234
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V. Zappalà, Ph. Bendjoya, A. Cellino, P. Farinella, C. Froeschlé, Icarus 116, 291 (1995).
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(1995)
Icarus
, vol.116
, pp. 291
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Zappalà, V.1
Bendjoya, P.2
Cellino, A.3
Farinella, P.4
Froeschlé, C.5
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17
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42549133363
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Whereas the Henan and Watsonia families are roughly the same distance from the sun, the mean orbits of asteroids making up these two families are markedly different in both eccentricity and inclination. The mean proper elements for the Henan family are ∼2.73 astronomical units (AU) (ranging from 2.69 to 2.76 AU), e ∼ 0.07, and sin(i) ∼ 0.06 (where e is eccentricity and i is inclination), compared with the Watsonia family at ∼2.77 AU (ranging from 2.74 to 2.80 AU), e ∼ 0.16, and sin(i) ∼0.29. This corresponds to a difference in orbital velocity between these families of over 6 km/s, making it highly unlikely these two families can be linked to a single parent body. 234 Barbara is a distinct asteroid located at 2.39 AU.
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Whereas the Henan and Watsonia families are roughly the same distance from the sun, the mean orbits of asteroids making up these two families are markedly different in both eccentricity and inclination. The mean proper elements for the Henan family are ∼2.73 astronomical units (AU) (ranging from 2.69 to 2.76 AU), e ∼ 0.07, and sin(i) ∼ 0.06 (where e is eccentricity and i is inclination), compared with the Watsonia family at ∼2.77 AU (ranging from 2.74 to 2.80 AU), e ∼ 0.16, and sin(i) ∼0.29. This corresponds to a difference in orbital velocity between these families of over 6 km/s, making it highly unlikely these two families can be linked to a single parent body. 234 Barbara is a distinct asteroid located at 2.39 AU.
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23
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42549096810
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To calculate the single-scattering albedo of each component, we employed Hapke's two-stream approximation assuming no opposition effect, isotropic scattering, and that all components have the same density and particle size (22). Once converted to single-scattering albedo, mixing is linear and relative abundances can be estimated using a least-squares solution (42, 43).
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To calculate the single-scattering albedo of each component, we employed Hapke's two-stream approximation assuming no opposition effect, isotropic scattering, and that all components have the same density and particle size (22). Once converted to single-scattering albedo, mixing is linear and relative abundances can be estimated using a least-squares solution (42, 43).
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24
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0028164393
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M. J. S. Belton et al., Science 265, 1543 (1994).
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(1994)
Science
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Belton, M.J.S.1
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25
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J. Veverka et al., Science 289, 2088 (2000).
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Science
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Veverka, J.1
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26
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H. Yano et al., Science 312, 1350 (2006).
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Science
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Yano, H.1
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27
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42549132123
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Asteroid spectra are routinely measured relative to a given wavelength, as in Fig. 3, where data are normalized to 0.55 μm. Absolute albedos are obtained from the Infrared Astronomical Satellite (IRAS) Supplemental IRAS Minor Planet Survey database, as archived in the NASA Planetary Data System data set IRAS-A-FPA-3-RDR-IMPS-V6.0.
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Asteroid spectra are routinely measured relative to a given wavelength, as in Fig. 3, where data are normalized to 0.55 μm. Absolute albedos are obtained from the Infrared Astronomical Satellite (IRAS) Supplemental IRAS Minor Planet Survey database, as archived in the NASA Planetary Data System data set IRAS-A-FPA-3-RDR-IMPS-V6.0.
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28
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42549111018
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Overall the asteroid spectra are red-sloped; i.e., they increase in reflectance with increasing wavelength. This is typical of asteroid spectra and generally thought to be related to either the presence of opaque phases or weathering in the space environment (44, 45).
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Overall the asteroid spectra are red-sloped; i.e., they increase in reflectance with increasing wavelength. This is typical of asteroid spectra and generally thought to be related to either the presence of opaque phases or weathering in the space environment (44, 45).
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29
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42549129742
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Although the spectrum of 2448 Sholokhov is not uniquely interpretable, its presence within the same family as several spinel-rich asteroids (the Watsonia family) makes it a stronger candidate for representing spectral slope in modeling these CAI-rich asteroids than any existing theoretical method or potential laboratory analog
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Although the spectrum of 2448 Sholokhov is not uniquely interpretable, its presence within the same family as several spinel-rich asteroids (the Watsonia family) makes it a stronger candidate for representing spectral slope in modeling these CAI-rich asteroids than any existing theoretical method or potential laboratory analog.
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37
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0037031697
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Y. Amelin, A. N. Krot, I. D. Hutcheon, A. A. Ulyanov, Science 297, 1678 (2002).
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Science
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Amelin, Y.1
Krot, A.N.2
Hutcheon, I.D.3
Ulyanov, A.A.4
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38
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0003444325
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C. Karr, Ed, Academic Press, San Diego, CA
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J. B. Adams, in Infrared and Raman Spectroscopy of Lunar and Terrestrial Materials, C. Karr, Ed. (Academic Press, San Diego, CA, 1975), pp. 91-116.
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W. F. Bottke Jr, A. Cellino, P. Paolicchi, R. P. Binzel, Eds, Univ. of Arizona Press, Tucson, AZ
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B. E. Clark, B. Hapke, C. Pieters, D. Britt, in Asteroids III, W. F. Bottke Jr., A. Cellino, P. Paolicchi, R. P. Binzel, Eds. (Univ. of Arizona Press, Tucson, AZ, 2003), pp. 585-599.
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(2003)
Asteroids III
, pp. 585-599
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Clark, B.E.1
Hapke, B.2
Pieters, C.3
Britt, D.4
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46
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42549108899
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This research was funded in part by NASA grants NNX06AH69G (J.M.S, NNG05GF39G (H.C.C, and NNG06GF56G (T.J.M. and L.M.L, and NSF grant AST-0307688 S.J.B, We thank T. Hiroi for carefully collecting our spectra of CAIs and Allende samples at RELAB, K. Domanik for assistance with the electron microprobe at Lunar and Planetary Laboratory, and R. Binzel and two anonymous reviewers for suggestions that improved this report. 518-520
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This research was funded in part by NASA grants NNX06AH69G (J.M.S.), NNG05GF39G (H.C.C.), and NNG06GF56G (T.J.M. and L.M.L.) and NSF grant AST-0307688 (S.J.B.). We thank T. Hiroi for carefully collecting our spectra of CAIs and Allende samples at RELAB, K. Domanik for assistance with the electron microprobe at Lunar and Planetary Laboratory, and R. Binzel and two anonymous reviewers for suggestions that improved this report. 518-520
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