报告题目：Turbulence and particle acceleration in collisionless magnetic reconnection
报告人：Dr. Lu San (卢三), Assistant Researcher at IGPP, UCLA
报告摘要：Magnetic reconnection is an important process in various plasma environments because it reconfigures the magnetic field and releases magnetic energy to accelerate charged particles. Recent spacecraft observations suggest that turbulence exists commonly in collisionless magnetic reconnection, which changes the reconnection process significantly. Using particle-in-cell simulation, we study turbulence and particle acceleration in collisionless magnetic reconnection, showing that (1) the turbulence is essentially caused by secondary islands in the reconnection region, (2) inhomogeneous temperature across the pre-reconnection current sheet favors formation of these secondary islands (i.e., the turbulence in reconnection), and (3) these secondary islands lead to a much more efficient energy conversion and particle acceleration. These simulation results are confirmed by ARTEMIS observations of magnetic reconnection in Earth’s magnetotail.
Dr. San Lu (firstname.lastname@example.org) is currently an assistant researcher in the Department of Earth, Planetary and Space Sciences at UCLA, USA. He received the B.S. degree in geophysics from University of Science and Technology of China in 2009, and the Ph.D. degree in space physics from University of Science and Technology of China in 2014.
From 2014 to 2015, he was working at University of Science and Technology of China as a postdoctoral researcher. Then he works at University of California, Los Angeles, USA as an assistant researcher from October 2015. He was also a visiting scholar at Auburn University, Auburn, USA from October 2012 to October 2013.
Dr. San Lu has ten years research experience of hybrid and particle-in-cell simulations of space plasma physics, especially on magnetospheric dynamics/kinetics. Now his research activities are mainly concerned with two fields:
(1) Magnetotail thin current sheet, magnetic reconnection, dipolarization fronts, magnetic islands (or flux ropes), particle acceleration and heating, and the dawn-dusk asymmetry using multi-spacecraft observations and particle-in-cell and hybrid simulations;
(2) Dayside kinetic/dynamic structure and processes (e.g., foreshock transients, flux transfer events) using three-dimensional dayside global hybrid simulations and spacecraft observations.