Elimination de colorants de l'industrie textile par des sciures de bois

L'élimination de la couleur de rejets de petites industries textiles peut être réalisée à l'aide de sciures d'essences de bois diverses dont le choix est fait après étude de leur relargage dans l'eau (couleur et DCO); les sciures de chêne, de châtaignier, de pin Douglas conduisent à des relargages de substances fortement colorées correspondant à des DCO d'environ 60 mg d'oxygène par gramme de sciures sèches et ceci en réacteur discontinu. Par contre, les sciures de hêtre, bouleau, sapin et peuplier relarguent nettement moins de produits colorés ou non et conduisent à des DCO plus faibles, excepté pour le bouleau (30 mg d'O2.g-1).Le pH de l'eau est également modifié par addition de sciures et l'on obtient des valeurs de pH d'équilibre atteint en 10 min., de 4,3; 5; 5,8 et 7 pour le bouleau, le sapin, le hêtre et le peuplier respectivement.L'élimination de colorants à 25 mg.l-1 dans l'eau par des doses de sciures de 50 g.-1 pour 2 h de temps de contact, montre qu'une meilleure décoloration (98 à 100 %) est obtenue pour le colorant cationique Basic Red 22 avec les quatre sciures sélectionnées, qu'avec les colorants anioniques (ou acides) dont les valeurs de rétention, variables selon les sciures (de 4 à 8 %) peuvent être très bonnes également.Les isothermes d'adsorption permettent de déterminer les capacités d'adsorption à saturation; à titre d'exemple, des valeurs de 0,1 à 0,2 mmol.g-1 sont obtenues sur des sciures de peuplier et de hêtre pour le colorant BR 22 et de 4 à 8.10- mmol.g-1 pour le colorant anionique Acid Blue 25, sur ces mêmes sciures. Contrairement à d'autres matériaux, on observe que les résultats obtenus ne dépendent que très peu de la température (entre 15 et 35 °C).Une étude dynamique sur colonne confirme les écarts pour les deux types de colorants, mais les résultats dépendent de la vitesse de passage : des pourcentages d'élimination de 0,4 à 1 % en masse peuvent être obtenus pour l'AB 25 le BR 22 sur la sciure de hêtre. Il faut cependant signaler que les produits minéraux et organiques contenus dans les effluents colorés industriels diminuent l'efficacité des sciures par rapport à leur efficacité sur des solutions de colorants purs.Anticipated water pollution regulations require textile dye industries to reduce substantially the amount of colour in their effluents. One possible method of colour removal is through adsorption techniques. The most commonly used adsorbent for treatment of textile effluents is activated carbon. The capability of sawdust for removing colour was recognised some time ago (POOTS et al. 1978; ABO-ELELA and EL-DIB, 1987; ASFOUR et al., 1985) as were those of peat and of charred woollen fiber treatments (PERINEAU et al., 1983). Sawdust has recently received more attention (ASFOUR et al., 1985) owing to its economic advantages when the sawmills are near the textile mills. In order to measure the real efficacy of some types of sawdust, evaluation of the released coloured products and their influence on the effluent water pH are never described. The aim of the present work is to study and evaluate the behaviour of types of sawdust from Limousin woods (released COD and pH of solutions) and the discolouring power of the selected sawdust (beech, poplar, birch and fir trees) with respect to textile dyes in dilute solutions and industrial effluents.MATERIALS AND METHODSExperiments were conducted using sawdust from beech, chestnut, poplar, oak, birch, fir and Douglas pine, in doses of 50 g.l-1 of water. The industrial sawdust particle site was between 0.5 - 1.5 mm.The dyestuffs used in all the experiments are reported in table 1. The initial concentration of colouring matter was 25 mg.l-1 and determined spectrophotometrically at maximum absorbance wavelength. In a batch system the time required for equilibrium was 2 hours (or less).RESULTS AND DISCUSSIONKinetic rejections of the sawdust are shown in figure 1; four types of sawdust are suitable : beech, poplar, birch, and fir were selected for further experiments. The absorbance depends on the wavelength and becomes maximum near UV range (as shown in fig. 2 and 3). The COD of the released products is particularly important for chestnut, oak, Douglas pine (60 mg.O2.g-1; table 2) and also for birch (31 mg.O2.g-1). These data have never been mentioned in published works where the wood was not submitted to any form of pre-treatment.Sawdust contains some acidic or basic groups that modify the pH of water (fig. 6, 7) which becomes more acidic; the phenomenon can be used to neutralize textile fixing effluents loaded with carbonate ions (pH : 10). Batch results (table 3) indicate that the tour selected types of sawdust give good colour removal for the 8 dyes; particularly, the cationic dye : Basic Red 22 is discoloured with very good yield (96 to 99.5 %) on beech and on birch sawdust.A variation of temperature between 15 and 35 °C does not change significantly the adsorption results and at pH = 2, the release decreases (table 2) and the adsorption increases (table 4).Equilibrium conditions of adsorption of basic and acidic dyes on four types of dust were studied using the Langmuir equation; this equation was also used for the determination of the « ultimate capacity » Г∞ and the equilibrium constant K (STUMM and MORGAN, 1981). The resulting Г∞ and K for some dyes (AB 25, BR 22, NLB) on fir, beech, poplar, and birch sawdust are given in table 5. The best results were obtained for the cationic dye BR 22 which showed an ultimate capacity of 0.210 and 0.06 mmol.g-1 on beech and on birch sawdust respectively. [The result for other dyes is in the order of 0.005 mmol.g-1]. The results obtained by extrapolation of the linearized Langmuir equation are somewhat different from those obtained by the experimental saturation curve (fig. 8) for BR 22 on polar sawdust. For AB 25, the saturation curve shows a great increase of the adsorption capacity for concentrated solutions (2 - 2.25 g.l-1), this is probably due to a micellary process as shown on figure 9 : the critical micellary concentration is between 1.5 and 3.3 g.1-1.DYNAMIC STUDYFlow tests using small columns (3 - 7 cm of height) are used with beech sawdust for determining the breakthrough curves (rate : 1.03 m.h-1). The concentrations of AB 25, BR 22 and their mixture are 25 mg.l-1 (close to industrial waste-water concentration). The adsorption capacity deduced from the « Bed Depth Service Time » model is 0.4 % and 0.8 % for each dye respectively.Glass columns (4 cm diameter) containing 20 g or 30 g of beech sawdust were also used. The values of adsorption for a rate of 3.1 m.h-1 are 0.45 mg.g-1 (0.04 %) for AB 25 and 13 mg.g-1 (1.3 %) for BR 22. Approximately 650 litres of this dye can be treated by this sawdust (fig. 10 and 11).Industrial effluents (unknown composition) are less discoloured, probably due to the presence of many other compounds.Batch experiments adsorption of dyes on wood sawdust can lead to different measurements of the efficiency of the sawdust depending on rejection by the adsorbent of chemical species in the bulk solution. These substances modify the pH, the adsorbance of the solution and the amount of adsorbed dyes by competitive reaction

Ground-based photometry of the 21-day Neptune HD106315c

Space-based transit surveys such as K2 and TESS allow the detection of small transiting planets with orbital periods beyond 10 days. Few of these warm Neptunes are currently known around stars bright enough to allow for detailed follow-up observations dedicated to their atmospheric characterization. The 21-day period and 3.95 $R_\oplus$ planet HD106315c has been discovered based on the observation of two of its transits by K2. We have observed HD106315 using the 1.2m Euler telescope equipped with the EulerCam camera on two instances to confirm the transit using broad band photometry and refine the planetary period. Based on two observed transits of HD106315c, we detect its $\sim$1 mmag transit and obtain a precise measurement of the planetary ephemerids, which are critical for planning further follow-up observations. We have used the attained precision together with the predicted yield from the TESS mission to evaluate the potential for ground-based confirmation of Neptune-sized planets found by TESS. We find that 1-meter-class telescopes on the ground equipped with precise photometers could substantially contribute to the follow-up of 162 TESS candidates orbiting stars with magnitudes of $V \leq 14$. Out of these, 74 planets orbit stars with $V \leq 12$ and 12 planets orbit $V \leq 10$, which makes these candidates high-priority objects for atmospheric characterization with high-end instrumentation.Comment: Published in A&A letters, 4 pages, 3 figure

A systematic typology for negative Poisson's ratio materials and the prediction of complete auxeticity in pure silica zeolite JST

© the Owner Societies 2015. Single crystals can commonly have negative Poisson's ratio in a few directions; however more generalised auxeticity is rarer. We propose a typology to distinguish auxetic materials. We characterise numerous single crystals and demonstrate that partial auxeticity occurs for around 37%. We find average auxeticity to be limited to α-cristobalite and no example of complete auxeticity. We simulate two hundreds pure silica zeolites with empirical potentials and quantum chemistry methods, and for the first time identify complete auxeticity in a zeolite network, JST

Decays of Ta182 and Ta183

The beta - decays of Ta182 and Ta183 into excited states of W182 and W183 have been studied using a curved crystal gamma-ray diffraction spectrometer and a homogeneous field, ring focusing beta-ray spectrometer. In each case de-excitation of the daughter nucleus gives rise to complex gamma-ray and conversion electron spectra. Energies and relative intensities of gamma rays and conversion lines arising from 27 transitions in W182 and 29 transitions in W183 are presented. Internal conversion coefficients and multipolarities have been deduced for most of the transitions and together with the gamma-ray energies form the basis of decay schemes proposed for both W182 and W183. The two decays are reported together because of the close experimental relationship which existed between them as a consequence of the method used for their production, namely, simultaneous production of Ta182 by single neutron capture and Ta183 by double neutron capture from stable Ta181. A corollary result is the value 1.3 x 10^4 barns for the thermal neutron cross section of Ta182. An interpretation of these results on W182 in terms of collective rotational motion has been given by A. Bohr and collaborators [Kgl. Danske Videnscab. Selskab, Mat.-fys. Medd. 29, No. 9 (1955)]

Rotational and intrinsic levels in Tm169 and Lu175

Nuclear levels in Tm169 excited by electron capture of Yb169, and levels in Lu175 excited by both beta decay of Yb175 and electron capture of Hf175 have been studied by using the curved-crystal gamma-ray spectrometer and the ring-focusing beta-ray spectrometer, as well as a semicircular beta-ray spectrometer for low energies. From the precision energies and the multipolarity determinations, the levels in Tm169 have the following energies in kev, and spin and parity assignments: A (ground state) (½+), B 8.42 (3/2+), C 118.20 (5/2+), D 138.95 (7/2+), E 316.19 (7/2+), F 379.31 (7/2-), G 472.91 (9/2-). Levels A, B, C, and D are members of a rotational band whose characteristic constants are given. Levels E and F are interpreted as particle excitations and level G as a rotational level based on the state F. The Lu175 excited states have the following energies in kev, spins, and parities: A (ground state) (7/2+), B 113.81 (9/2+), C 251.46 (11/2+), D 343.40 (5/2+), E 396.31 (9/2-), F 432.76 (7/2+), G 504.7 (1/2+). A, B, and C form a rotational band for which the characteristic constants are given. Some features of the levels and transition probabilities are discussed and compared with the unified model. A brief survey of second-order rotational energy constants and of intrinsic excitation levels is given

Determination of the anisotropic elastic properties of rocksalt Ge2Sb2Te5 by XRD, residual stress, and DFT

© 2016 American Chemical Society. The chalcogenide material Ge2Sb2Te5 is the prototype phase-change material, with widespread applications for optical media and random access memory. However, the full set of its independent elastic properties has not yet been published. In this study, we determine the elastic constants of the rocksalt Ge2Sb2Te5, experimentally by X-ray diffraction (XRD) and residual stress and computationally by density functional theory (DFT). The stiffnesses (XRD-stress/DFT) in GPa are C11 = 41/58, C12 = 7/8, and C44 = 8/12, and the Zener ratio is 0.46/0.48. These values are important to understand the effect of elastic distortions and nonmelting processes on the performances of increasingly small phase change data bits

Gamma Transitions in W182

[No abstract]

The CORALIE survey for southern extrasolar planets. XVI. Discovery of a planetary system around HD 147018 and of two long period and massive planets orbiting HD 171238 and HD 204313

We report the detection of a double planetary system around HD 140718 as well as the discovery of two long period and massive planets orbiting HD 171238 and HD 204313. Those discoveries were made with the CORALIE Echelle spectrograph mounted on the 1.2-m Euler Swiss telescope located at La Silla Observatory, Chile. The planetary system orbiting the nearby G9 dwarf HD 147018 is composed of an eccentric inner planet (e=0.47) with twice the mass of Jupiter (2.1 MJup ) and with an orbital period of 44.24 days. The outer planet is even more massive (6.6 MJup) with a slightly eccentric orbit (e=0.13) and a period of 1008 days. The planet orbiting HD 171238 has a minimum mass of 2.6 MJup, a period of 1523 days and an eccentricity of 0.40. It orbits a G8 dwarfs at 2.5 AU. The last planet, HD 204313 b, is a 4.0 MJup -planet with a period of 5.3 years and has a low eccentricity (e = 0.13). It orbits a G5 dwarfs at 3.1 AU. The three parent stars are metal rich, which further strengthened the case that massive planets tend to form around metal rich stars.Comment: 6 pages, 6 figures, accepted for publication in A&

Comparing HARPS and Kepler surveys: The alignment of multiple-planet systems

Aims. We study a subset of the planetary population characterized both by HARPS and Kepler surveys. We compare the statistical properties of planets in systems with m.sin i >5-10 M_Earth and R>2 R_Earth. If we assume that the underlying population has the same characteristics, the different detection sensitivity to the orbital inclination relative to the line of sight allows us to probe the planets' mutual inclination. Methods. We considered the frequency of systems with one, two and three planets as dictated by HARPS data. We used Kepler's planetary period and host mass and radii distributions (corrected from detection bias) to model planetary systems in a simple yet physically plausible way. We then varied the mutual inclination between planets in a system according to different prescriptions (completely aligned, Rayleigh distributions and isotropic) and compared the transit frequencies with one, two or three planets with those measured by Kepler. Results. The results show that the two datasets are compatible, a remarkable result especially because there are no tunable knobs other than the assumed inclination distribution. For m.sin i cutoffs of 7-10 M_Earth, which are those expected to correspond to the radius cutoff of 2 R_Earth, we conclude that the results are better described by a Rayleigh distribution with mode of 1 deg or smaller. We show that the best-fit scenario only becomes a Rayleigh distribution with mode of 5 deg if we assume a rather extreme mass-radius relationship for the planetary population. Conclusions. These results have important consequences for our understanding of the role of several proposed formation and evolution mechanisms. They confirm that planets are likely to have been formed in a disk and show that most planetary systems evolve quietly without strong angular momentum exchanges (abridged).Comment: 10 pages, 6 figures, 4 tables, accepted for publication in Astronomy & Astrophysic