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TIMOTHY G MATTSON Timothy G Mattson earned a PhD in chemistry from the University of California at Santa Cruz for his work on quantum molecular scattering theory This was followed by a postdoc at Caltech where he ported his molecular scattering software to the Caltech/JPL hypercubes Since then, he has held a number of commercial and academic positions with computational science on high performance computers as the common thread He has been involved with a number of noteworthy projects in parallel computing, including the ASCI Red project (the first TeraFLOP MPP), the creation of OpenMP, and OSCAR (a popular package for cluster computing) Currently he is responsible for Intel's strategy for the life sciences market and is Intel's chief spokesman to the life sciences community BEVERLY A SANDERS Beverly A Sanders received a PhD in applied mathematics fr om Harvard University She has held faculty positions at the University of Maryland, the Swiss Federal Institute of Technology (ETH Zurich), and Caltech, and is currently with the Department of Computer and Information Science and Engineering at the University of Florida A main theme of her teaching and research has been the development and application of techniques, including design patterns, formal methods, and programming language concepts, to help programmers construct high quality, correct programs particularly programs involving concurrency BERNA L MASSINGILL Berna L Massingill earned a PhD in computer science from Caltech This was followed by a postdoc at the University of Florida, where she and the other authors began their work on design patterns for parallel computing She currently holds a faculty position in the Department of Computer Science at Trinity University (San Antonio, Texas) She also spent more than ten years as a working programmer, first in mainframe systems programming and later as a developer for a software company Her research interests include parallel and distributed computing, design patterns, and formal methods, and a goal of her teaching and research has been applying ideas from these fields to help programmers construct high quality, correct programs.

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Using Barcode encoder for Visual Studio .NET Control to generate, create barcode image in Visual tudio .NET applications.already be open, but if not, select this page by clicking on the correct Toolbox Page button The Button control will be easy to nd as the controls appear in alphabetical order When you double-click on it, a new button will ppear at the top left of the form, as shown in Figure A16 Now add a Label to the form in the same way Currently both controls will occupy the same location at the top left of the form Drag each of the controls to a more central location, with the label near the centre of the form and the button below it Con gure the Button and Label As with the form, the Button and Label will both have a number of default settings that need to be changed to make it appear and behave as you would wish The Properties window is again used, but this time, before you change any properties, you must make sure that the correct control is selected (click on a control and draghandles will appear around it) The currently selected control (or if none is selected, the form) is the one that the Properties window will interact with Change the button s Name property to btnHello, and its Text property to Hello Change the Label s Name to lblHello, and its Text to nothing (ie delete the current text Label1, but do not replace it with any text).Related: 

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The temporal variation of p ( ) of R CrB itself was observed by Coyne & Shawl (1973) during a photometric minimum Very signi cant developments in the spectral behaviour were recorded, these being interpreted as dramatic changes in the distribution of particles of different sizes associated with the discrete cloud model Further observations were presented by Coyne (1974), which supported the model Spectropolarimetric observations have been made of V 854 Cen by Kameswara Rao & Raveendran (1993) They noted that the p ( ) variation was much steeper during the light minimum During the brightness decline phase, the polarized ux was attenuated by the same factor as the ux directly from the star, this implying that the obscuring cloud affects both the radiation from the photosphere and the scattering centres, suggesting a restriction to the geometrical extent of the scattering region In an observational study of the global values of p in a collection of objects in the stages of evolution from red giant to planetary nebula, Johnson & Jones (1991) noted that polarization is a characteristic of the majority of these stars When arranged on an evolutionary sequence, a clear trend in p was found A maximum of polarization was observed within an evolutionary stage The value of p was found to increase with age from mildly dusty Mira variables, through to protoplanetary nebulae for which the highest polarization is found; the polarization then decreases as the star evolves into an old planetary nebula Spectropolarimetry of 31 post-asymptotic giant branch (post-AGB) stars were observed by Trammell, Dinerstein & Goodrich (1994), these objects believed to be in the rst phases of the transition from the AGB to the planetary nebula stage Their survey suggested that the objects might be placed into one of four types depending on the recorded behaviour of p ( ) and ( ) Type [1] objects display higher levels of polarization and large position angle rotations; Type [2] have polarizations too large to be attributed to interstellar material, but without large position angle changes; Type [3] objects show position angle rotations and polarization changes across TiO absorption features; Type [4] are bjects for which the observed polarization can be entirely attributed to interstellar effects Twenty four objects displayed evidence for aspherical geometry, with an implication that asymmetry begins very early in the transition from AGB to the planetary nebula phase Their schematic model involves bipolar lobes giving rise to polarization in the blue part of the spectrum as a result of scattering of photospheric light by the contained dust grains Orthogonal to these lobes is an obscuring torus, and the polarization in the red is the result of scattering of photospheric light or transmission polarization in this torus Likkel, Morris, Kastner, et al (1994) have obtained maps of IRAS 21282+5050 revealing that the polarization is not centro-symmetric close into the stellar source It was concluded that there is not a large component of scattered light in the nearinfrared The emission at 22 m may arise from transiently heated dust In a polarimetric study of IRC +10216, a carbon-rich infrared evolved star on the AGB of the HR diagram, Kastner & Weintraub (1994) found elliptical symmetry in a J-band map endorsing other photometric maps, all these providing evidence of axial symmetry of the envelope, with the equatorial plane of the star lying perpendicular to the major axis of the surrounding inner envelope of the nebula The axisymmetric.

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