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Kauffmann, Philipp,Cordesmeyer, Robert,Fouellefack, Gisele Awondzeko,Schminke, Boris,Wiese, Karl-Gunther Korean Association of Maxillofacial Plastic and Re 2018 Maxillofacial Plastic Reconstructive Surgery Vol.40 No.-
Background: Clefts in newborns are associated with severe morphological and functional impairment. Especially the lip is of importance as if the treatment result is unsatisfactory, it can lead to psychological changes in the patient. Different operative procedures have been developed over the last decades. The aim of the presented study was the comparison of the surgical techniques according to Millard and Pfeifer regarding the temporal development of the postoperative symmetry of the lip height and mouth width. Methods: Digitized photographs of patients from the department of oral and maxillofacial surgery at the University of Göttingen were evaluated from 1979 to 1996. With a video analysis program, the lip height and mouth width were analyzed regarding the symmetry. We demonstrated the symmetry values over a period of 8 years in order to show the influence of growth on postoperative results. Results: The development of the vertical symmetry of the Philtrum and the lip vermillion on the cleft side in comparison to the healthy side behaves differently depending on Pfeifer and Millard. The lip height of the cleft lip was shorter in both techniques than on the healthy side, but Pfeifer's difference was significantly more pronounced. The lip vermillion height on the cleft side was slightly shorter in the Millard group and markedly larger in the Pfeifer group. Both techniques can achieve good symmetry results for the vertical dimension of the lip. According to Pfeifer, the development of the horizontal dimension on the cleft side is bigger within the first 4 years than on the healthy side; according to the Millard technique, the horizontal development is smaller. These differences are greater within the first 6 years and approach between the 6th and 8th year. Conclusions: The Millard technique demonstrates better results concerning the philtrum and vermillion symmetry during growth within the first 6 years. Over the whole study period, growth corrects the philtrum and vermillion symmetry within the Pfeifer group.
Confirmation of the VeLLO L1148−IRS: star formation at very low (column) density
Kauffmann, J.,Bertoldi, F.,Bourke, T. L.,Myers, P. C.,Lee, C. W.,Huard, T. L. Blackwell Publishing Ltd 2011 Monthly notices of the Royal Astronomical Society Vol.416 No.3
<P><B>ABSTRACT</B></P><P>We report the detection of a compact (∼5 arcsec; about 1800 au projected size) CO outflow from L1148−IRS. This confirms that this <I>Spitzer</I> source is physically associated with the nearby (≈325 pc) L1148 dense core. Radiative transfer modelling suggests an internal luminosity of 0.08 to 0.13 L<SUB>⊙</SUB>. This validates L1148−IRS as a Very Low Luminosity Object (VeLLO; <I>L</I>≤ 0.1 L<SUB>⊙</SUB>). The L1148 dense core has unusually low densities and column densities for a star‐forming core. It is difficult to understand how L1148−IRS might have formed under these conditions. Independent of the exact final mass of this VeLLO (which is likely <0.24 M<SUB>⊙</SUB>), L1148−IRS and similar VeLLOs might hold some clues about the isolated formation of brown dwarfs.</P>
Microstructure evolution in Alloy 617 B after a long-term creep and thermal aging at 700°C
Speicher, Magdalena,Kauffmann, Florian,Shim, Jae-Hyeok,Chandran, Mahesh Elsevier 2018 Materials science & engineering. properties, micro Vol.711 No.-
<P><B>Abstract</B></P> <P>Changes in the microstructure of heat-resistant materials may influence their long-term behaviour. For this reason, materials chosen for high temperature-based applications, e.g. advanced ultra-supercritical (A-USC) steam power plants, must exhibit long-term microstructure stability. Therefore, changes in the microstructure of frequently used materials must be determined and correlated with their creep behaviour to assure a reliable operation of components. In this work, a long-term study investigated the microstructure of a creep rupture specimen made of a nickel-based alloy 617 B. The creep tests were carried out at 700°C for up to 45,148h. By using optical microscopy (OM), scanning electron microscopy (SEM) and transmission electron microscopy (TEM) the virgin, thermal-loaded and creep states were characterized. The precipitate location, number and size have been determined. The experiment results were compared, discussed and correlated to the creep and failure behaviour. Furthermore, the long-term precipitation kinetics of Alloy 617 B was simulated, which considered its thermal history, using the MatCalc software. The simulated precipitates fraction and size were compared with the experimental data obtained in this study. The comparison between the experimental and simulation results demonstrated comparable gamma prime (γ') phases. The simulation results of the carbides identified at the grain boundaries were satisfactory. However, the size of the intragranular fine carbides M<SUB>23</SUB>C<SUB>6</SUB> was not reproduced correctly.</P>
Oscillatory Mass Transport in Vapor-Liquid-Solid Growth of Sapphire Nanowires
Oh, S. H.,Chisholm, M. F.,Kauffmann, Y.,Kaplan, W. D.,Luo, W.,Ruhle, M.,Scheu, C. American Association for the Advancement of Scienc 2010 Science Vol.330 No.6003
<P>In vapor-liquid-solid (VLS) growth, the liquid phase plays a pivotal role in mediating mass transport from the vapor source to the growth front of a nanowire. Such transport often takes place through the liquid phase. However, we observed by in situ transmission electron microscopy a different behavior for self-catalytic VLS growth of sapphire nanowires. The growth occurs in a layer-by-layer fashion and is accomplished by interfacial diffusion of oxygen through the ordered liquid aluminum atoms. Oscillatory growth and dissolution reactions at the top rim of the nanowires occur and supply the oxygen required to grow a new (0006) sapphire layer. A periodic modulation of the VLS triple-junction configuration accompanies these oscillatory reactions.</P>
<i>GALEX</i>-SDSS CATALOGS FOR STATISTICAL STUDIES
Budavá,ri, Tamá,s,Heinis, Sé,bastien,Szalay, Alexander S.,Nieto-Santisteban, Marí,a,Gupchup, Jayant,Shiao, Bernie,Smith, Myron,Chang, Ruixiang,Kauffmann, Guinevere,Morrissey, P IOP Publishing 2009 The Astrophysical journal Vol.694 No.2
CARMA LARGE AREA STAR FORMATION SURVEY: DENSE GAS IN THE YOUNG L1451 REGION OF PERSEUS
Storm, Shaye,Mundy, Lee G.,Lee, Katherine I.,Ferná,ndez-Ló,pez, Manuel,Looney, Leslie W.,Teuben, Peter,Arce, Hé,ctor G.,Rosolowsky, Erik W.,Meisner, Aaron M.,Isella, Andrea,Kauffmann American Astronomical Society 2016 The Astrophysical journal Vol.830 No.2
<P>We present a 3 mm spectral line and continuum survey of L1451 in the Perseus Molecular Cloud. These observations are from the CARMA Large Area Star Formation Survey (CLASSy), which also imaged Barnard. 1, NGC 1333, Serpens Main, and Serpens South. L1451 is the survey region with the lowest level of star formation activity-it contains no confirmed protostars. HCO+, HCN, and N2H+ (J = 1 -> 0). are all detected throughout the region, with HCO+ being the most spatially widespread, and molecular emission seen toward 90% of the area above N(H-2) column densities of 1.9 x 10(21) cm(-2). HCO+ has the broadest velocity dispersion, near 0.3 km s(-1) on average, compared with similar to 0.15 km s(-1) for the other molecules, thus representing a range of subsonic to supersonic gas motions. Our non-binary dendrogram analysis reveals that the dense gas traced by each molecule has a similar hierarchical structure, and that gas surrounding the candidate first hydrostatic core (FHSC), L1451-mm, and other previously detected single-dish continuum clumps has similar hierarchical structure; this suggests that different subregions of L1451 are fragmenting on the pathway to forming young stars. We determined that the three-dimensional morphology of the largest detectable dense-gas structures was relatively ellipsoidal compared with other CLASSy regions, which appeared more flattened at the largest scales. A virial analysis shows that the most centrally condensed dust structures are likely unstable against collapse. Additionally, we identify a new spherical, centrally condensed N2H+ feature that could be a new FHSC candidate. The overall results suggest that L1451 is a young region starting to form its generation of stars within turbulent, hierarchical structures.</P>