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Die Bestimmung von Lipoprotein(a) im Plasma mittels kinetischer Nephelometrie (Beckman Instruments) wurde mit einem immunoradiometrischen Assay (Mercodia) verglichen. Untersucht wurden 182 Proben in frischem Zustand und 18 Proben, die für kurze Zeit bei -25 °C gelagert waren. Die Meßergebnisse zeigen eine gute Übereinstimmung der Median werte (147 mg/1 bzw. 160 mg/1) und eine gute Korrelation bei den frischen und den eingefrorenen Proben (r = 0,971/rs= 0,985 bzw. r = 0,971). Die Variationskoeffizienten der Nephelometrie entsprechen mit 4.2% in der Serie (Intraassay) und 5,5-6,5% von Tag zu Tag (Interassay) den bisherigen Literaturwerten. Entgegen der Empfehlung, nur frisches Probenmaterial für die Nephelometrie einzusetzen, wurde bei einer Probe mit einer hohen Lipoprotein(a) Konzentration (960 mg/1) über 5 Wochen keine bedeutende Abnahme der Meßwerte registriert. Um den Einfluß der Triglyzeridkonzentration auf die Lp(a) Bestimmung zu untersuchen, wurden sechs Plasmaproben mit Triglyzeridwerten > 5,75 mmol/1 ausgewählt und in verschiedenen Verdünnungen mit Triglyzeridkonzentrationen zwischen 3,45-8,05 mmol/1 analysiert. Während 4 Proben keinen Einfluß der Triglyzeridkonzentration zeigten, wurde bei 2 Proben ein geringer Abfall der Lipoprotein(a) Meßwerte mit steigender Triglyzeridkonzentration beobachtet.
We investigate the structure of the potential energy surfaces of the superheavy nuclei 158258Fm100, 156264Hs108, 166278112, 184298114, and 172292120 within the framework of self-consistent nuclear models, i.e., the Skyrme-Hartree-Fock approach and the relativistic mean-field model. We compare results obtained with one representative parametrization of each model which is successful in describing superheavy nuclei. We find systematic changes as compared to the potential energy surfaces of heavy nuclei in the uranium region: there is no sufficiently stable fission isomer any more, the importance of triaxial configurations to lower the first barrier fades away, and asymmetric fission paths compete down to rather small deformation. Comparing the two models, it turns out that the relativistic mean-field model gives generally smaller fission barriers.
We study the extrapolation of nuclear shell structure to the region of superheavy nuclei in self-consistent mean-field models—the Skyrme-Hartree-Fock approach and the relativistic mean-field model—using a large number of parametrizations which give similar results for stable nuclei but differ in detail. Results obtained with the folded-Yukawa potential which is widely used in macroscopic-macroscopic models are shown for comparison. We focus on differences in the isospin dependence of the spin-orbit interaction and the effective mass between the models and their influence on single-particle spectra. The predictive power of the mean-field models concerning single-particle spectra is discussed for the examples of 208Pb and the spin-orbit splittings of selected neutron and proton levels in 16O, 132Sn, and 208Pb. While all relativistic models give a reasonable description of spin-orbit splittings, all Skyrme interactions show a wrong trend with mass number. The spin-orbit splitting of heavy nuclei might be overestimated by 40%–80%, which exposes a fundamental deficiency of the current nonrelativistic models. In most cases the occurrence of spherical shell closures is found to be nucleon-number dependent. Spherical doubly magic superheavy nuclei are found at 184298114, 172292120, or 184310126 depending on the parametrization. The Z=114 proton shell closure, which is related to a large spin-orbit splitting of proton 2f states, is predicted only by forces which by far overestimate the proton spin-orbit splitting in 208Pb. The Z=120 and N=172 shell closures predicted by the relativistic models and some Skyrme interactions are found to be related to a central depression of the nuclear density distribution. This effect cannot appear in macroscopic-microscopic models or semiclassical approaches like the extended Thomas-Fermi-Strutinski integral approach which have a limited freedom for the density distribution only. In summary, our findings give a strong argument for 172292120 to be the next spherical doubly magic superheavy nucleus.