Différences
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| Les deux révisions précédentesRévision précédenteProchaine révision | Révision précédente | ||
| animation:workshops:2013:plasma [2013/04/19 12:11] – sbarends | animation:workshops:2013:plasma [2013/04/26 13:52] (Version actuelle) – [Shocks, Reconnection, and Particle Acceleration in Plasma-fluids] sbarends | ||
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| Centre Blaise Pascal, ENS-Lyon, France | Centre Blaise Pascal, ENS-Lyon, France | ||
| - | June 20-21, 2013 \\ | + | June 20-21, 2013 \\ |
| [[http:// | [[http:// | ||
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| Organizing committee: | Organizing committee: | ||
| * **Rolf Walder**, CRAL, École normale supérieure de Lyon | * **Rolf Walder**, CRAL, École normale supérieure de Lyon | ||
| - | * **Christophe Winisdoerffer**, | + | |
| + | * **Andrei Bykov**, Ioffe Institute, Russian Academy of Sciences, St. Petersburg, Russia | ||
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| + | * **Mickaël Melzani**, CRAL, École normale supérieure de Lyon, France | ||
| Administrative coordination: | Administrative coordination: | ||
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| The workshop is supported by: | The workshop is supported by: | ||
| - | * Centre Blaise Pascal | + | * **CBP** - Centre Blaise Pascal, Lyon, France |
| - | * FLMSN | + | |
| - | * CRAL | + | |
| + | * **ENSL** - École normale supérieure de Lyon | ||
| + | * **Université de Lyon** | ||
| + | * **CNRS** - Centre National de la Recherche Scientifique | ||
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| ===== Summary ===== | ===== Summary ===== | ||
| - | The acceleration of non-thermal particles in large scale flows is of prime importance in astrophysics and beyond, for example in earth science where high-energy cosmic rays likely have a strong | + | The acceleration of non-thermal particles in large scale flows is of prime importance in astrophysics and beyond. Cosmic accelerators can energize particles up to 10²⁰ eV. The flux of high-energy cosmic rays has a strong |
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| + | However, accelerators embedded in large scale MHD flows within astrophysical objects still remain enigmatic | ||
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| + | The first day concentrates on theoretical questions of plasma physics, particle acceleration, | ||
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| + | The second day presents results of modeling concrete astrophysical objects: microquasars and X-ray binaries, pulsars and their winds, gamma-ray bursts, solar wind, supernova remnants and superbubbles, | ||