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Astrophysical reconnection and collisionless dissipation

机译：天体重新连接和无碰撞耗散

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摘要

Magnetic reconnection and collisionless dissipation are common phenomena of astrophysical and fusion plasmas. While reconnection is responsible for disruptions of a fusion confinement, it causes flare explosions at the Sun and stars, in galaxies, planetary magnetospheres, and it causes aurorae and structure formation in the Universe as well as penetration through magnetic boundaries. Due to the weak coupling in astrophysical and fusion plasmas, dissipation is due to collective phenomena such as plasma waves and micro-turbulence rather than direct particle-particle collisions. Since astrophysical plasmas usually are not directly observable, laboratory investigations may help to verify theoretical plasma astrophysical predictions but for the transfer of knowledge one has to take into account some specifies of astroplasmas, their density, temperature, currents and magnetic field strengths, geometry and even topology. As an example we discuss magnetic reconnection in the solar corona which requires collisionless dissipation. Both are highly nonlinear processes that occur at totally different scales. Hence, we refer to numerical simulations. Finally, we list the most urgent open questions in plasma astrophysics which should be addressed in the near future.
机译：磁重连接和无碰撞耗散是天体物理和聚变等离子体的普遍现象。重新连接虽然造成了聚变禁闭的破坏，但它会在太阳和恒星，星系，行星磁层的火星爆炸，并导致宇宙中的极光和结构形成以及穿过磁边界的穿透。由于天体物理和聚变等离子体之间的耦合较弱，耗散是由于诸如等离子体波和微湍流之类的集体现象，而不是直接的粒子-粒子碰撞。由于天体物理等离子体通常不可直接观察到，因此实验室研究可能有助于验证理论上的天体物理预测，但对于知识的转移，必须考虑到天体的某些特定规定，其密度，温度，电流和磁场强度，几何形状甚至拓扑。作为示例，我们讨论需要无碰撞耗散的日冕中的磁重连接。两者都是高度非线性的过程，发生在完全不同的规模上。因此，我们指的是数值模拟。最后，我们列出了等离子天体物理学中最紧迫的悬而未决的问题，应在不久的将来解决。

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