scholarly journals X-ray nanotomography uncovers morphological heterogeneity in a polymerization catalyst at multiple reaction stages

2021 ◽  
Author(s):  
Maximilian J. Werny ◽  
Roozbeh Valadian ◽  
Leon M. Lohse ◽  
Anna-Lena Robisch ◽  
Silvia Zanoni ◽  
...  
2017 ◽  
Vol 95 (4) ◽  
pp. 363-370 ◽  
Author(s):  
Jianlong Sun ◽  
David J. Berg ◽  
Brendan Twamley

The synthesis of tetrabenzo[a,c,g,i]fluorenyl (Tbf) yttrium dialkyl complexes, (Tbf)Y(CH2SiMe3)2(L) (L = tetrahydrofuran (THF), 1; L = bipy, 2), by direct protonolysis of the tris(alkyl) complex, Y(CH2SiMe3)3(THF)2, are reported. The X-ray crystal structures of 1 and 2 display the helical twisting typically observed for the Tbf ligand. Dynamic nuclear magnetic resonance (NMR) studies on 1 show a barrier to Tbf helical inversion (epimerization or “wagging”) of 38.1 ± 0.5 kJ mol−1. The reaction of 1 with acidic hydrocarbons such as 1,3-bis(trimethylsilyl)cyclopentadiene or trimethylsilylacetylene results in protonolysis to form the mixed Cp derivative [(Tbf){C5H3(SiMe3)2}Y(CH2SiMe3)(THF)] (3) or [(Tbf)Y(CCSiMe3)2(THF)]n (4), respectively. In the case of 4, a small amount of the trinuclear cluster (Tbf)Y3(μ3-CCSiMe3)2(μ2-CCSiMe3)3(CCSiMe3)3(THF)2 (5) was isolated and characterized by X-ray crystallography. Dialkyl 1 undergoes smooth insertion of trimethylsilyl isocyanate to afford [(Tbf)Y{κ2-(N,O)-Me3SiN(Me3SiCH2)CO}2(THF)] (6) but it does not react with alkenes. Treating 1 with [Ph3C]+[B(C6F5)4]− in bromobenzene generates a moderately active ethylene polymerization catalyst (36 kg mol−1 h−1 bar−1).


Polyhedron ◽  
1995 ◽  
Vol 14 (1) ◽  
pp. 1-10 ◽  
Author(s):  
Ying Mu ◽  
Warren E. Piers ◽  
Leonard R. Macgillivray ◽  
Michael J. Zaworotko

Clay Minerals ◽  
2002 ◽  
Vol 37 (3) ◽  
pp. 465-471 ◽  
Author(s):  
Seung Yeop Lee ◽  
Soo Jin Kim

AbstractThe morphological and structural changes in smectite caused by hexadecyltrimethylammonium (HDTMA) treatment were studied using X-ray diffraction (XRD) and transmission electron microscopy (TEM). The HDTMA-exchanged smectite shows not only morphological features such as irregular, wavy surface with curled edges, but also structural features such as large d-spacings (20 – 26 Å ) and lattice distortions. The surface morphological heterogeneity is assumed to be related to the inhomogeneous intercalation of HDTMA cations into the interlayer of smectite.


Catalysts ◽  
2019 ◽  
Vol 9 (4) ◽  
pp. 303 ◽  
Author(s):  
Rosa Arrigo ◽  
Manfred Schuster

Wet impregnation is broadly applied for the synthesis of carbon-supported metal/metal oxide nanostructures because of its high flexibility, simplicity and low cost. By contrast, impregnated catalysts are typified by a usually undesired nanostructural and morphological heterogeneity of the supported phase resulting from a poor stabilization at the support surface. This study on graphite-supported Fe-based materials from an Fe nitrate precursor is concerned with the understanding of the chemistry that dictates during the multistep synthesis, which is key to designing structurally homogeneous catalysts. By means of core-level X-ray photoelectron spectroscopy, near-edge X-ray absorption fine structure spectroscopy and atomic resolution electron microscopy, we found not only a large variety of particles sizes and morphologies but also chemical phases. Herein, thermally stable single atoms and few atoms clusters are identified together with large agglomerates of an oxy-hydroxide ferrihydrite-like phase. Moreover, the thermally induced phase transformation of the initially poorly ordered oxy-hydroxide phase into several oxide phases is revealed, together with the existence of thermally stable N impurities retained in the structure as Fe–N–O bonds. The nature of the interactions with the support and the structural dynamics induced by the thermal treatment rationalize the high heterogeneity observed in these catalysts.


2017 ◽  
Vol 63 (5) ◽  
pp. 325-328
Author(s):  
Pavel O. Rumyantsev ◽  
Aleksandr Yu. Abrosimov ◽  
Aleksandr S. Tertychnyi ◽  
Liliya S. Selivanova ◽  
Konstantin Yu. Slashchuk

We present a clinical case of rare and poorly diagnosable mediastinal teratoma containing elements of mature pancreas tissue, nesidioblastosis, and focal hyperplasia of neuroendocrine cells in a somatically healthy 25-year-old male. The main diagnostic difficulties are associated with the asymptomatic clinical course of mediastinal teratomas that are usually incidentally discovered during X-ray for other conditions. The pathology is characterized by pronounced morphological heterogeneity of the tumor; if the morphologist is not sufficiently qualified, this often results in a false-positive conclusion of neuroendocrine carcinoma, which, in turn, leads to an inadequate amount of treatment and a wrong prognosis in the patient. Therefore, for verification of the diagnosis, histological specimens should be examined by experts of institutions experienced in morphological differential diagnosis. In this case, an immunohistochemical study of the tumor for insulin, cytokeratins, and markers of neuroendocrine differentiation as well as measurement of the proliferation index Ki-67 in several areas are the key tests. This pathology is extremely rare, which leads to numerous misdiagnoses.


1994 ◽  
Vol 144 ◽  
pp. 275-277
Author(s):  
M. Karlický ◽  
J. C. Hénoux

AbstractUsing a new ID hybrid model of the electron bombardment in flare loops, we study not only the evolution of densities, plasma velocities and temperatures in the loop, but also the temporal and spatial evolution of hard X-ray emission. In the present paper a continuous bombardment by electrons isotropically accelerated at the top of flare loop with a power-law injection distribution function is considered. The computations include the effects of the return-current that reduces significantly the depth of the chromospheric layer which is evaporated. The present modelling is made with superthermal electron parameters corresponding to the classical resistivity regime for an input energy flux of superthermal electrons of 109erg cm−2s−1. It was found that due to the electron bombardment the two chromospheric evaporation waves are generated at both feet of the loop and they propagate up to the top, where they collide and cause temporary density and hard X-ray enhancements.


1994 ◽  
Vol 144 ◽  
pp. 1-9
Author(s):  
A. H. Gabriel

The development of the physics of the solar atmosphere during the last 50 years has been greatly influenced by the increasing capability of observations made from space. Access to images and spectra of the hotter plasma in the UV, XUV and X-ray regions provided a major advance over the few coronal forbidden lines seen in the visible and enabled the cooler chromospheric and photospheric plasma to be seen in its proper perspective, as part of a total system. In this way space observations have stimulated new and important advances, not only in space but also in ground-based observations and theoretical modelling, so that today we find a well-balanced harmony between the three techniques.


1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.


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