セッション概要

宇宙惑星科学(P) セッション小記号 太陽地球系科学・宇宙電磁気学・宇宙環境(EM) セッションID P-EM10 タイトル 和文 Wave, Turbulence, Reconnection, and Energetic Particles in Solar, Space and Laboratory 英文 Wave, Turbulence, Reconnection, and Energetic Particles in Solar, Space and Laboratory タイトル短縮名 和文 turbulence, reconnection and particles 英文 turbulence, reconnection and particles 代表コンビーナ 氏名 和文 Yan Huirong 英文 Huirong Yan 所属 和文 Kavli Institute of Astronomy & Astrophysics 英文 Kavli Institute of Astronomy & Astrophysics メールアドレス hryan@pku.edu.cn 共同コンビーナ 1 氏名 和文 Takeru Suzuki 英文 Takeru Suzuki 所属 和文 Department of Physics, School of Science, Nagoya University 英文 Department of Physics, School of Science, Nagoya University メールアドレス stakeru@nagoya-u.jp 共同コンビーナ 2 氏名 和文 Alex Lazarian 英文 Alex Lazarian 所属 和文 University of Wisconsin-Madison 英文 University of Wisconsin-Madison メールアドレス alazarian@wisc.edu 国際セッション開催希望 国際セッションとしての開催を希望する 発表主要言語 英語 スコープ 和文 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. 英文 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. 発表方法希望 口頭および（または）ポスターセッション 招待講演 Jungyeon Cho Gregogz Kowal Nikolai Pogorelov Reinhard Schlickeiser Bo Li