H2 productivity. However, Ni-MOF-74 is unstable under reaction conditions and forms metallic nickel particles. To improve catalyst activity and stability, bimetallic (NixMg1-x)-MOF-74 catalysts were developed that stabilize the Ni OMS and promote the dehydrogenation reaction. An optimal composition exists at (Ni0.32Mg0.68)-MOF-74 that gives the greatest H2 productivity, up to 203 mL gcat-1 min-1 at 300 °C, and maintains 100% selectivity to CO and H2 between 225–275 °C. The optimized catalyst is also active for the dehydrogenation of other alcohols. DFT calculations reveal that synergistic interactions between the open metal site and the organic linker lead to lower reaction barriers in the MOF catalysts compared to the open metal site alone. This work expands the suite of hydrogen-related reactions catalyzed by MOF-74 which includes recent work on hydroformulation and our earlier reports of aryl-ether hydrogenolysis. Moreover, it highlights the use of bimetallic frameworks as an effective strategy for stabilizing a high density of catalytically active open metal sites.
Empirical recurrent relations, governing the structure of the devil’s staircase in the driven Chua’s circuit are given, which reflect the self-similar structure in an algebraic form. In particular, it turns out that the same formulas hold for both winding and period numbers, but with different “initial conditions”. Some of the finer details such as period-doubling along with numerous coexistence phenomena within staircases of mode-locked states have been revealed by computing high-resolution bifurcation diagrams.
The mechanism of wear-particle formation during unlubricated sliding wear of several carbon and alloy steels has been investigated by scanning (SEM) and transmission electron microscopy (TEM). Individual debris particles are plate-like and typically 200 to 400 nm in thickness. The thinner particles are generally iron oxides except at low temperatures or in inert atmospheres when predominantly metallic particles result. The mean debris-particle width was 1 to 2 ..mu..m. TEM revealed a fine dislocation cell structure typical of large strain deformation to a depth of 10 to 50 ..mu..m. The subsurface cell dimensions and bending of pearlite colonies indicate that the shear strain near to the surface is at least 5. In many instances, a 200 to 300 nm wide zone of lower dislocation density, indicative of recovery, we noted immediately below the surface. Some cracks formed along dislocation cell walls at the boundary of the recovered zone; others were associated with decohesion of particle interfaces of subgrain triple points. Some oxidation then occurs during separation of the platelet from the parent material as a consequence of the highly pyrophoric nature of thin metal flakes. The sequence of the dry sliding wear process is discussed. 16 figures.
An entry from the Cambridge Structural Database, the world’s repository for small molecule crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the CCDC and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.
No abstract is provided for this article.
Metallicity is expected to influence not only the lives of massive stars but also the outcome of their deaths as supernovae (SNe) and as gamma-ray bursts (GRBs). However, there are surprisingly few direct measurements of the local metallicities of different flavors of core-collapse SNe. Here we present the largest existing set of host-galaxy spectra with H II region emission lines at the sites of 34 stripped-envelope core-collapse SNe. We derive local oxygen abundances in a robust manner in order to constrain the SN Ib/c progenitor population. We obtain spectra at the SN sites, include SNe from targeted and untargeted surveys, and perform the abundance determinatinos using three different oxygen-abundance calibrations. The sites of SNe Ic (the demise of the most heavily stripped stars having lost both the H and He layers) are systematically more metal rich than those of SNe Ib (arising from stars that retained their He layer) in all calibrations. A Kolmogorov-Smirnov-test yields a very low probability of 0.1% that SN Ib and SN Ic environment abundances, which are different on average by 0.2 dex (in the Pettini & Pagel scale), are drawn from the same parent population. Broad-lined SNe Ic (without GRBs) occur at metallicities between those of SNe Ib and SNe Ic. Lastly, we find that the host-galaxy central oxygen abundance, widely inferred from the host-galaxy luminosity, is not a good indicator of the local SN metallicity; hence, large-scale SN surveys need to obtain local abundance measurements in order to quantify the impact of metallicity on stellar death.
Ga[OSi(O<sup>t</sup>Bu)<sub>3</sub>]<sub>3</sub>·THF was used as the first thermolytic single-source molecular precursor to generate gallium-containing silicas.