2,912 research outputs found

    Знання як фактор конкурентних переваг: перспективи України

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    Introduction. In recent decades, economic growth of the leading world countries have occurred on the basis of information and knowledge embodied in new products, production technologies and management at all stages of production and marketing. Due to the generation and commercialisation of knowledge competitive advantages of individual companies, institutions and national economies, leaders of economic growth are formed and advanced. Considering the current trends in the changing conditions of economic and political space of Ukraine and abroad, which will only intensify fast and efficient reorientation to new markets is relevant for the domestic producers. The purpose of the study is to investigate the role and place of knowledge as an element of intellectual capital of organisations to ensure their competitiveness in light of trends in the global economy; to assess the current position and to outline the problems and perspectives of fast and efficient innovation growth in Ukraine based on knowledge. Results. The role of knowledge in providing competitive advantages of organisations has been outlined. The place of knowledge relevant to intellectual capital of organisations is specified. It has been determined that knowledge as an element of intellectual capital has a dual nature: it can be regarded both as an intellectual resource and as a possibility to implement existing intellectual capital of organisations. The influence of knowledge in the global economy is investigated. Ukraine’s position in the world rankings, which reflects the level of economic development based on intellectual capital and innovation, as well as the status of its competitiveness, has been studied. From these positions, we have specified strengths and weaknesses of the national economy and outlined the prospects of economic growth based on knowledge as an element of intellectual capital.Окреслено роль знань у забезпеченні конкурентних переваг організацій. Уточнено місце знань в інтелектуальному капіталі організації. Визначено, що знання як елемент інтелектуального капіталу, мають дуалістичну природу: їх можна розглядати як інтелектуальний ресурс, а також як можливість реалізації наявного інтелектуального капіталу організації. Досліджено вплив знань на розвиток світової економіки. Досліджено позиції України у світових рейтингах, які відображають рівень економічного розвитку країн на основі інтелектуального капіталу та інновацій, а також стан їхньої конкурентоспроможності. Визначено сильні та слабкі сторони вітчизняної економіки, а також окреслено проблеми та перспективи її зростання на основі знань як елементу інтелектуального капіталу

    S-DIMM+ height characterization of day-time seeing using solar granulation

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    To evaluate site quality and to develop multi-conjugative adaptive optics systems for future large solar telescopes, characterization of contributions to seeing from heights up to at least 12 km above the telescope is needed. We describe a method for evaluating contributions to seeing from different layers along the line-of-sight to the Sun. The method is based on Shack Hartmann wavefront sensor data recorded over a large field-of-view with solar granulation and uses only measurements of differential image displacements from individual exposures, such that the measurements are not degraded by residual tip-tilt errors. We conclude that the proposed method allows good measurements when Fried's parameter r_0 is larger than about 7.5 cm for the ground layer and that these measurements should provide valuable information for site selection and multi-conjugate development for the future European Solar Telescope. A major limitation is the large field of view presently used for wavefront sensing, leading to uncomfortably large uncertainties in r_0 at 30 km distance.Comment: Accepted by AA 22/01/2010 (12 pages, 11 figures

    Are Panel Unit Root Tests Useful for Real-Time Data?

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    With the development of real-time databases, N vintages are available for T observations instead of a single realization of the time series process. Although the use of panel unit root tests with the aim to gain in efficiency seems obvious, empirical and simulation results shown in this paper heavily mitigate the intuitive perspective.macroeconomics ;

    Exploring the temporally resolved electron density evolution in EUV induced plasmas

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    We measured for the first time the electron density in an Extreme Ultra-Violet induced plasma. This is achieved in a low-pressure argon plasma by using a method called microwave cavity resonance spectroscopy. The measured electron density just after the EUV pulse is 2.610162.6\cdot10^{16} m3^{-3}. This is in good agreement with a theoretical prediction from photo ionization, which yields a density of 4.510164.5\cdot10^{16} m3^{-3}. After the EUV pulse the density slightly increase due to electron impact ionization. The plasma (i.e. electron density) decays in tens of microseconds.Comment: 3 pages, 4 figure

    Measurements of plasma motions in dynamic fibrils

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    We present a 40 minute time series of filtergrams from the red and the blue wing of the \halpha line in an active region near the solar disk center. From these filtergrams we construct both Dopplergrams and summed ``line center'' images. Several dynamic fibrils (DFs) are identified in the summed images. The data is used to simultaneously measure the proper motion and the Doppler signals in DFs. For calibration of the Doppler signals we use spatially resolved spectrograms of a similar active region. Significant variations in the calibration constant for different solar features are observed, and only regions containing DFs have been used in order to reduce calibration errors. We find a coherent behavior of the Doppler velocity and the proper motion which clearly demonstrates that the evolution of DFs involve plasma motion. The Doppler velocities are found to be a factor 2--3 smaller than velocities derived form proper motions in the image plane. The difference can be explained by the radiative processes involved, the Doppler velocity is a result of the local atmospheric velocity weighted with the response function. As a result the Doppler velocity originates from a wide range in heights in the atmosphere. This is contrasted by the proper motion velocity which is measured from the sharply defined bright tops of the DFs and is therefore a very local velocity measure. The Doppler signal originates from well below the top of the DF. Finally we discuss how this difference together with the lacking spatial resolution of older observations have contributed to some of the confusion about the identity of DFs, spicules and mottles.Comment: 8 pages, 7 figures, Accepted in ApJ, see http://www.astro.uio.no/~oysteol for better quality figures and mpg movi

    Numerical Simulations of Shock Wave-Driven Jets

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    We present the results of numerical simulations of shock wave-driven jets in the solar atmosphere. The dependence of observable quantities like maximum velocity and deceleration on parameters such as the period and amplitude of initial disturbances and the inclination of the magnetic field is investigated. Our simulations show excellent agreement with observations, and shed new light on the correlation between velocity and deceleration and on the regional differences found in observations.Comment: 7 pages, 11 figures, submitted to Ap

    Dynamic fibrils in H-alpha and C IV

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    Aim: To study the interaction of the solar chromosphere with the transition region, in particular active-region jets in the transition region and their relation to chromospheric fibrils. Methods: We carefully align image sequences taken simultaneously in C IV with the Transition Region and Coronal Explorer and in H-alpha with the Swedish 1-m Solar Telescope. We examine the temporal evolution of "dynamic fibrils", i.e., individual short-lived active-region chromospheric jet-like features in H-alpha. Results: All dynamic fibrils appear as absorption features in H-alpha that progress from the blue to the red wing through the line, and often show recurrent behavior. Some of them, but not all, appear also as bright features in C IV which develop at or just beyond the apex of the H-alpha darkening. They tend to best resemble the H-alpha fibril at +700 mA half a minute earlier. Conclusions: Dynamic chromospheric fibrils observed in H-alpha regularly correspond to transition-region jets observed in the ultraviolet. This correspondence suggests that some plasma associated with dynamic fibrils is heated to transition-region temperatures.Comment: 8 pages, 8 figure

    Polynomial algebras and exact solutions of general quantum non-linear optical models I: Two-mode boson systems

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    We introduce higher order polynomial deformations of A1A_1 Lie algebra. We construct their unitary representations and the corresponding single-variable differential operator realizations. We then use the results to obtain exact (Bethe ansatz) solutions to a class of 2-mode boson systems, including the Boson-Einstein Condensate models as special cases. Up to an overall factor, the eigenfunctions of the 2-mode boson systems are given by polynomials whose roots are solutions of the associated Bethe ansatz equations. The corresponding eigenvalues are expressed in terms of these roots. We also establish the spectral equivalence between the BEC models and certain quasi-exactly solvable Sch\"ordinger potentials.Comment: 20 pages, final version to appear in J. Phys. A: Math. Theor

    Striation and convection in penumbral filaments

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    Observations with the 1-m Swedish Solar Telescope of the flows seen in penumbral filaments are presented. Time sequences of bright filaments show overturning motions strikingly similar to those seen along the walls of small isolated structures in the active regions. The filaments show outward propagating striations with inclination angles suggesting that they are aligned with the local magnetic field. We interpret it as the equivalent of the striations seen in the walls of small isolated magnetic structures. Their origin is then a corrugation of the boundary between an overturning convective flow inside the filament and the magnetic field wrapping around it. The outward propagation is a combination of a pattern motion due to the downflow observed along the sides of bright filaments, and the Evershed flow. The observed short wavelength of the striation argues against the existence of a dynamically significant horizontal field inside the bright filaments. Its intensity contrast is explained by the same physical effect that causes the dark cores of filaments, light bridges and `canals'. In this way striation represents an important clue to the physics of penumbral structure and its relation with other magnetic structures on the solar surface. We put this in perspective with results from the recent 3-D radiative hydrodynamic simulations.Comment: Accepted for publication in A&
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