白雪宁，2007年本科毕业于清华大学基础科学班，2012年于普林斯顿大学获得天体物理博士学位。2012-2017年在哈佛-史密松天体物理中心理论与计算天体物理研究所（ITC）作为哈勃学者和ITC学者开展独立博士后研究，期间作为讲师在哈佛大学讲授等离子体天体物理课程。他2017年加入清华大学高等研究院任研究员，2019年起兼职于清华大学天文系，2023年起任长聘教授。他主要从事理论和计算天体物理研究，主要研究方向包括原行星盘和行星形成，以及等离子体天体物理，特别是同宇宙线相关的物理过程，并为此开发相应的计算方法和数值工具。Cosmic-rays are energetic charged particles. Their origin, transport and feedback of are of fundamental importance over a wide range of astrophysical systems. Typically, the kinetic physics of the CRs lies in their gyro-scale and above, while conventional kinetic simulation methods require resolving much smaller microscopic scales of the background plasmas. This issue can be substantially alleviated thanks to the development of the magnetohydrodynamic-particle-in-cell (MHD-PIC) method, and its extension to integrate particles under the guiding-center approximation. Using such methods, I will describe our efforts in studying fundamental plasma astrophysics problems including 1). Particle acceleration in shocks and turbulence; 2). The CR gyro-resonant instabilities and measurement of transport coefficients of low-energy (GeV) CRs, which are the key to understanding CR feedback at galactic scales; 3). Non-relativistic magnetic reconnection.