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Why hybrid porous solids capture greenhouse gases?
Fé,rey, Gé,rard,Serre, Christian,Devic, Thomas,Maurin, Guillaume,Jobic, Hervé,Llewellyn, Philip L.,De Weireld, Guy,Vimont, Alexandre,Daturi, Marco,Chang, Jong-San Royal Society of Chemistry 2011 Chemical Society reviews Vol.40 No.2
<P>Hybrid porous solids, with their tunable structures, their multifunctional properties and their numerous applications, are currently topical, particularly in the domain of adsorption and storage of greenhouse gases. Most of the data reported so far concern the performances of these solids in this domain, particularly in terms of adsorbed amounts of gas but do not explain at the atomic level why and how adsorption and storage occur. From a combination of structural, spectroscopic, thermodynamic experiments and of molecular simulations, this <I>tutorial review</I> proposes answers to these open questions with a special emphasis on CO<SUB>2</SUB> and CH<SUB>4</SUB> storage by some rigid and flexible hybrid porous materials.</P> <P>Graphic Abstract</P><P>Why and how hybrid porous solids capture gases: exploration combining appropriate <I>in situ</I> measurements and molecular simulations. <IMG SRC='http://pubs.rsc.org/services/images/RSCpubs.ePlatform.Service.FreeContent.ImageService.svc/ImageService/image/GA?id=c0cs00040j'> </P>
Hydrogen Storage in the Giant-Pore Metal–Organic Frameworks MIL-100 and MIL-101
Latroche, Michel,Surblé,, Suzy,Serre, Christian,Mellot-Draznieks, Caroline,Llewellyn, Philip L.,Lee, Jin-Ho,Chang, Jong-San,Jhung, Sung Hwa,Fé,rey, Gé,rard WILEY-VCH Verlag 2006 Angewandte Chemie Vol.45 No.48
<B>Graphic Abstract</B> <P>Large hydrogen-storage capacity at liquid-nitrogen temperature is exhibited by the metal–organic framework MIL-101. In the zeotype architecture of this porous solid (see picture) each intersection of the cages is occupied by a supertetrahedron formed by trimers of chromium octahedra assembled with benzene-1,4-dicarboxylate ligands. <img src='wiley_img/14337851-2006-45-48-ANIE200600105-content.gif' alt='wiley_img/14337851-2006-45-48-ANIE200600105-content'> </P>
A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb
Miyake, N.,Sumi, T.,Dong, Subo,Street, R.,Mancini, L.,Gould, A.,Bennett, D. P.,Tsapras, Y.,Yee, J. C.,Albrow, M. D.,Bond, I. A.,Fouqué,, P.,Browne, P.,Han, C.,Snodgrass, C.,Finet, F.,Furusawa, K IOP Publishing 2011 The Astrophysical journal Vol.728 No.2
<P>We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 +/- 0.02) x 10(-4) and a separation of d = 0.97537 +/- 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t(E), and angular Einstein radius,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.</P>
Schmitt, Fé,lix,Banu, Rajesh,Yeom, Ick-Tae,Do, Khac-Uan Elsevier 2018 Biochemical engineering journal Vol.133 No.-
<P><B>Abstract</B></P> <P>An artificial neural network (ANN) was first developed to predict the transmembrane pressure in an anoxic-aerobic membrane bioreactor (AO-MBR) treating domestic wastewater. A few studies about prediction of membrane fouling in MBRs using ANNs have been published so far, even though our recent work indicates that ANNs show a great potential for this application. In this study, 10 parameters linked to wastewater treatment and measured in the different parts of the AO-MBR system were used as the input variables of the ANN. The goal was to select the most relevant input parameters to predict the evolution of the transmembrane pressure based on the performances of the ANN. An ANN model was selected for its satisfying performances (<I>R</I> <SUP>2</SUP> = 0.850). In conclusion, ANNs could be a valid method to predict membrane fouling in AO-MBR systems treating domestic wastewater.</P> <P><B>Highlights</B></P> <P> <UL> <LI> A set of ANNs is first developed to predict membrane fouling in AO-MBR. </LI> <LI> An optimal set of parameters was identified to predict TMP using ANN efficiently. </LI> <LI> High performances were reached (R<SUP>2</SUP> = 0.850) for the developed ANN. </LI> <LI> ANN model have shown high potential to predict membrane fouling. </LI> </UL> </P>
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III
Dawson, Kyle S.,Schlegel, David J.,Ahn, Christopher P.,Anderson, Scott F.,Aubourg, É,ric,Bailey, Stephen,Barkhouser, Robert H.,Bautista, Julian E.,Beifiori, Alessandra,Berlind, Andreas A.,Bhardw IOP Publishing 2013 The Astronomical journal Vol.145 No.1
Kostov, V. B.,McCullough, P. R.,Hinse, T. C.,Tsvetanov, Z. I.,Hé,brard, G.,Dí,az, R. F.,Deleuil, M.,Valenti, J. A. IOP Publishing 2013 The Astrophysical journal Vol.770 No.1
<P>We report the discovery of a transiting, gas giant circumbinary planet orbiting the eclipsing binary KIC 4862625 and describe our independent discovery of the two transiting planets orbiting Kepler-47. We describe a simple and semi-automated procedure for identifying individual transits in light curves and present our follow-up measurements of the two circumbinary systems. For the KIC 4862625 system, the 0.52 +/- 0.018 R-Jupiter radius planet revolves every similar to 138 days and occults the 1.47 +/- 0.08 M-circle dot, 1.7 +/- 0.06 R-circle dot F8 IV primary star producing aperiodic transits of variable durations commensurate with the configuration of the eclipsing binary star. Our best-fit model indicates the orbit has a semi-major axis of 0.64 AU and is slightly eccentric, e = 0.1. For the Kepler-47 system, we confirm the results of Orosz et al. Modulations in the radial velocity of KIC 4862625A are measured both spectroscopically and photometrically, i.e., via Doppler boosting, and produce similar results.</P>
Lee, Young Hoon,Kristopo, Hari,Woo, Arim,Won, Mi Seon,Hayami, Shinya,Thué,ry, Pierre,Jung, Ok-Sang,Lee, Hong In,Kim, Bok Jo,Lindoy, Leonard F.,Kim, Yang CSIRO Publishing 2012 Australian journal of chemistry Vol.65 No.7
<P> Two new polyamine ligands, L1 and L2, incorporating pyridyl and aliphatic amine donor sites have been prepared and their reaction with copper(ii) yields the mono- and binuclear complexes [Cu(L1)](ClO4)2 (1) and [Cl2Cu(L2)CuCl(H2O)]ClO4 (2), respectively. The X-ray structure of 1 confirms that the five nitrogen donors of L1 are bound to the central copper ion to give a distorted square pyramidal coordination sphere. In 2, L2 acts as a bridging ligand with its N3-donor coordination domains separated by a m-xylylene spacer group. An unusual feature of this latter complex is that symmetrical L2 gives rise to non-equivalent coordination behaviour at the individual copper sites; while both sites display five-coordination with distorted square pyramidal arrangements, they differ in having N3Cl2- and N3ClO-donor atom sets, respectively. The electron paramagnetic resonance (EPR) spectra of both complexes are discussed. Variable temperature magnetic susceptibility data confirmed the absence of magnetic interactions in 1 while a weak antiferromagnetic interaction between copper(ii) centres occurs in 2. </P>
Satellite content and quenching of star formation in galaxy groups at<i>z</i>~ 1.8
Gobat, R.,Daddi, E.,Bé,thermin, M.,Pannella, M.,Finoguenov, A.,Gozaliasl, G.,Le Floc’h, E.,Schreiber, C.,Strazzullo, V.,Sargent, M.,Wang, T.,Hwang, H. S.,Valentino, F.,Cappelluti, N.,Li, Y.,Hasi EDP Sciences 2015 Astronomy and astrophysics Vol.581 No.-