A KOMATIITE SUCCESSION AS AN ANALOG FOR THE OLIVINE BEARING ROCKS AT JEZERO
A.J BrownR. C. WiensS. MauriceKyle UckertMike TiceDavid FlanneryA. H. TreimanK. L. SiebachL. W. BeegleWilliam AbbeyJ. F. BellL. E. MayhewJustin I. SimonO. BeyssacPeter A. WillisR. BhartiaR. J. SmithThierry FouchetCathy Quantin‐NatafP. PinetLucia MandonStéphane Le MouélicArya UdryB. HorganF. J. CalefE. A. CloutisNathalie TurenneClément RoyerMarìa‐Paz ZorzanoEleni RavanisS. A. FagentsAlberto González FairénSanjeev GuptaV. SautterYang LiuM. E. SchmidtKeyron Hickman‐Lewis
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B-containing olivine from the Tayozhnoye Fe deposit (Siberia, Russia) has unusually high H and F contents of 0.012 H and 0.026-0.043 F per formula unit of four O atoms.
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3672 cm^(-1) has not been observed in previously published olivine spectra. Transmission electron microscopy indicates substantial replacement of olivine by clinohumite and disordered mixtures of olivine and humite-group minerals near the rims of the olivine grains, whereas the interiors of the olivine grains contain regions of unaltered olivine structure. H_2O contents calculated from the defect stoichiometry and defect density are approximately
one-tenth of the total H_2O content estimated from the infrared data. The O-H bands, therefore, are believed to reflect the presence of OH within the olivine crystal
structure. Infrared-active stretching vibrations at 758, 1164, and 1257 cm^(-1) are consistent with the presence of [4]BO_4 groups within the olivine structure. Our data represent the first direct evidence of the coupled substitution B(F,OH)Si_(-1),O_(-1), in orthosilicate minerals. As a potential carrier of B, F, and H in the subducted oceanic lithosphere, olivine may play
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This study examines family farms and characteristics affecting farm succession. Based on a farm survey, three aspects of succession are analysed in the paper: the probability of family succession; the likelihood of having a successor designated; and the timing of succession. Large and specialised farms are more likely to be transferred within the family and to have appointed a successor. The number of family members, as well as the experience of farm operator, is also significantly related to the succession behaviour. The probabilities of succession, and of having a successor, first increase with age and then decline again. Furthermore, timing of succession is delayed as the farm holder ages, suggesting most farm operators' succession plans to be inconsistent over time. In addition, we find a significant interrelationship between the different aspects of succession indicating that decisions on family succession, the designation of a successor, as well as the timing of succession, are not separable.
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Abstract An attempt has been made to examine the extent to which seasonal periodicity of lacustrine phytoplankton corresponds to the general concepts of the theory of ecological succession. The study was carried out on an eutrophic lake (Aydat, France). As R EYNOLDS (1980, 1984) suggests, the seasonal periodicity of phytoplankton is an autogenic succession which may be perturbed by allogenic physical processes that change the initial direction of the succession. Thus, in this lake, only spring succession of phytoplankton can be considered as a true succession, consistent with the theory of ecological succession in that it was a directional and predictable phenomenon leading to an increasing complexity of community.
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The nationally-recognized Susquehanna
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The recent acquisition of high resolution 0.3 - 2.6 micron reflectance spectra for a number of olivine-rich asteroids permits the analysis of their surface compositions to be made on the basis of new and existing laboratory spectral data for pallasitic olivines and olivine-metal mixtures. Analysis of the spectral data for the latter has revealed a number of spectral parameters which can be used to constrain olivine and metal abundances, grain sizes, and olivine compositions. The following topics are discussed in greater detail: pallasite olivine spectra, olivine-metal mixture spectra, and olivine-rich asteroid spectra.
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