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The top documents tagged [magnetic pressure]
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Seed Population for Particle Acceleration... Anywhere in the Universe Shock heating based on many factors: 1. 1. v shock : shock speed 2. 2. Bn : magnetic
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Chapter 7 The Structure and the Origin of the Solar System والشمس وضحاها والشمس تجري لمستقر لها ذلك تقدير العزيز العليم ومن آياته
217 views
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Instrumental & Technical Requirements. Science objectives for helioseismology Understanding the interaction of the p-mode oscillations and the solar magnetic
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17 th Real-Time Conference | Lisboa, 24-28 May 2010 Plasma Control @ COMPASS a Vertical Solution H. Fernandes, IPFN and IPP.cz CODAC team 1 Instituto de
213 views
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Model Photospheres
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May 2008 - Ljubljana Magnetic Field Upper Limits for Jet Formation in X-ray binaries & AGNs M. Kaufman Bernadó 1,* & M. Massi 1 1 Max Planck Institut für
214 views
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The CME Link to Filaments and Filament Channels
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By: Rose Zimmerman. Main Points Shape Classification Properties Large Magellanic Cloud Small Magellanic Cloud Dwarf Irregular Galaxy Stars
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Predicting Solar Energetic Particle Events John Davis, Ron Moore, Edward West, Allen Gary NASA/MSFC/NSSTC Solar and Space Physics and the Vision for Space
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D.A. Yager-Elorriaga , S.G. Patel, A.M. Steiner, N.M. Jordan, R.M. Gilgenbach , and Y.Y. Lau
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I. INTRODUCTION Gas Pressure Magnetic Tension Coronal loops are thin and bright structure of hot plasma emitting intense radiation in X-ray and EUV. (1)
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3D simulations of solar emerging flux ISOBE Hiroaki Plasma seminar 2004/04/28
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