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W. PERRET,R. THATER,U. ALBER,C. SCHWENK,M. RETHMEIER 한국자동차공학회 2011 International journal of automotive technology Vol.12 No.6
Fusion welding processes are widely used for joining metal structures, such as pipes, ships, and cars. In general, these joining processes offer a very good compromise between reliability, safety, cost and maintenance which are important issues in the current economical context. The negative heat effects of welding, i.e. distortions and residual stresses of the welded parts, are well known and many researches in this field have already been done in the last decades in order to minimize them. On the experimental side, many sophisticated procedures have become state of the art to deal with this problem. On the computational side, the improvement of the simulation algorithms and the computing power enables the simulations of many physical phenomena occurring during the welding process. The implementation of welding simulation techniques is nevertheless not an easy task and often associated with expert knowledge which hinders their global application in an industrial environment. This paper is focused on the industrial requirements of a welding simulation software with special respect to the needs of the automotive industry. The necessary information to run a welding simulation and the expectations of a weld specialist without deep knowledge in numerical methods are investigated. These expectations are tested on an automotive welded assembly with a commercially available welding simulation software designed especially for the needs of the automotive industry. A welding experiment is done and the measured temperature distributions and distortions serve as reference to validate the simulation results. The result quality of the simulations of temperature fields and distortions is in best agreement with experimental data. The workflow is well adapted for the considered industrial requirements and the time-tosolution as well as the computational costs are acceptable, whereas the efficient calibration of the heat input model is still a point which will be further investigated in current and future research works.
Quantitative four-dimensional tracking of cytoplasmic and nuclear HIV-1 complexes
Arhel, Nathalie,Genovesio, Auguste,Kim, Kyeong-Ae,Miko, Sarah,Perret, Emmanuelle,Olivo-Marin, Jean-Christophe,Shorte, Spencer,Charneau, Pierre Nature Publishing Group 2006 Nature methods Vol.3 No.10
Emerging real-time techniques for imaging viral infections provide powerful tools for understanding the dynamics of virus-host cell interactions. Here we labeled human immunodeficiency virus-1 (HIV-1) integrase with a small tetracysteine tag, which preserved the virus' infectivity while allowing it to be labeled with the bis-arsenical fluorescein derivative FlAsH. This labeling allowed us to image both intracytoplasmic and intranuclear HIV-1 complexes in three dimensions over time (4D) in human cells and enabled us to analyze HIV-1 kinetics by automated 4D quantitative particle tracking. In the cytoplasm, HIV-1 complexes underwent directed movements toward the nuclear compartment, kinetically characteristic of both microtubule- and actin-dependent transport. The complexes then adopted smaller movements in a very confined volume once associated with the nuclear membrane and more diffuse movements once inside the nucleus. This work contributes new insight into the various movements of HIV-1 complexes within infected cells and provides a useful tool for the study of virus-host cell interactions during infection.
An extremely young massive clump forming by gravitational collapse in a primordial galaxy
Zanella, A.,Daddi, E.,Le Floc’h, E.,Bournaud, F.,Gobat, R.,Valentino, F.,Strazzullo, V.,Cibinel, A.,Onodera, M.,Perret, V.,Renaud, F.,Vignali, C. Nature Publishing Group, a division of Macmillan P 2015 Nature Vol.521 No.7550
When cosmic star formation history reaches a peak (at about redshift z ≈ 2), galaxies vigorously fed by cosmic reservoirs are dominated by gas and contain massive star-forming clumps, which are thought to form by violent gravitational instabilities in highly turbulent gas-rich disks. However, a clump formation event has not yet been observed, and it is debated whether clumps can survive energetic feedback from young stars, and afterwards migrate inwards to form galaxy bulges. Here we report the spatially resolved spectroscopy of a bright off-nuclear emission line region in a galaxy at z = 1.987. Although this region dominates star formation in the galaxy disk, its stellar continuum remains undetected in deep imaging, revealing an extremely young (less than ten million years old) massive clump, forming through the gravitational collapse of more than one billion solar masses of gas. Gas consumption in this young clump is more than tenfold faster than in the host galaxy, displaying high star-formation efficiency during this phase, in agreement with our hydrodynamic simulations. The frequency of older clumps with similar masses, coupled with our initial estimate of their formation rate (about 2.5 per billion years), supports long lifetimes (about 500 million years), favouring models in which clumps survive feedback and grow the bulges of present-day galaxies.