2014年4月29日(火) 14:15 〜 16:00 414 (4F)

コンビーナ:*Yan Huirong(Kavli Institute of Astronomy & Astrophysics)、Takeru Suzuki(Department of Physics, School of Science, Nagoya University)、Alex Lazarian(University of Wisconsin-Madison)、座長:Yan Huirong(Kavli Institute of Astronomy & Astrophysics)

Magnetized plasmas are frequently filled with waves and turbulence in both space and laboratory. In the context of solar and space physics, wave and turbulence play a critical role in generating the Sun's magnetic field, heating its atmosphere to millions of Kelvin, driving the solar wind, picking up the newly ionized ions, and in interpreting the Voyager data at and beyond the edge of the Heliosphere. Waves transport energy to different regions and their dissipation directly leads to heating plasmas. In the heating of the solar wind, compressible processes have recently been paid much attention in the dissipation of Alfvenic turbulence. Also, particle transport is determined by turbulence. Recent advances in understanding MHD turbulence induce substantial changes in the understanding of cosmic ray transport in turbulent magnetic field. In addition, turbulence enables fast magnetic reconnection and magnetic reconnection has shown the ability to accelerate energetic particles efficiently. We aim at creating a forum for experts to summarize recent significant advances in the corresponding fields and to discuss new directions. We cordially seek for the contributions from experts of these several directions in particular: a) How compressibility is important in the dissipation of Alfvenic turbulence b) How turbulence changes the properties of magnetic reconnection; c) Feedback of magnetic reconnection on turbulence in magnetized plasmas;d) Particle acceleration in turbulence and reconnection. The need for laboratory plasma physicists to participate is essential. Their work has proven very helpful to bridge the gap between theory and what happens in natural settings. Experiments can model collisionality regimes ranging from moderately collisionless to quite collisional. 3D data sets, with spatial resolution down below the MHD dissipation scale, can be used to evaluate reconnecting, turbulent hierarchies of scales both in space and in time.