氟是核天体物理学中最感兴趣的元素之一。长期以来，渐近巨星分支（Asymptotic Giant Branch，AGB）中的氟超丰问题一直难以用天体物理标准模型来解释。基于锦屏深地核天体物理实验装置（Jinping Underground laboratory for Nuclear Astrophysics，JUNA），利用强流加速器和高效的4π BGO探测器直接测量了AGB星中氟破坏反应¹⁹F（p，αγ）¹⁶O。将¹⁹F（p，αγ）¹⁶O反应的测量推进到有史以来最低的72.4 keV，测量结果覆盖了整个天体物理感兴趣的伽莫夫能区，与之前的理论外推差异很大，且不确定度得到了极大降低，为天体物理模型计算提供了可靠的核物理输入量。

中国原子能科学研究院核天体物理研究组在HI-13串列加速器核物理国家实验室建成了我国首条低能放射性次级束流线，产生了从⁶He到²²Na等11种放射性核束，利用这些放射性束流通过测量逆运动学转移反应开展了一系列核天体物理重要反应的研究，另外还通过厚靶实验方法和电荷交换反应开展了天体物理相关重要核结构信息的研究。在串列加速器Q3D磁谱仪上，利用稳定束测量了许多单核子转移和α基团转移的角分布，基于渐进归一化系数（Asymptotic Normalization Coefficient，ANC）或谱因子方法得到了一系列天体物理关键反应的天体物理S因子和反应率，为元素丰度、天体模型等相关研究提供了重要实验依据。

A new approach to target development for laboratory astrophysics experiments at high-power laser facilities is presented. With the dawn of high-power lasers, laboratory astrophysics has emerged as a field, bringing insight into physical processes in astrophysical objects, such as the formation of stars. An important factor for success in these experiments is targetry. To date, targets have mainly relied on expensive and challenging microfabrication methods. The design presented incorporates replaceable machined parts that assemble into a structure that defines the experimental geometry. This can make targets cheaper and faster to manufacture, while maintaining robustness and reproducibility. The platform is intended for experiments on plasma flows, but it is flexible and may be adapted to the constraints of other experimental setups. Examples of targets used in experimental campaigns are shown, including a design for insertion in a high magnetic field coil. Experimental results are included, demonstrating the performance of the targets.

We report on the design and first results from experiments looking at the formation of radiative shocks on the Shenguang-II (SG-II) laser at the Shanghai Institute of Optics and Fine Mechanics in China. Laser-heating of a two-layer CH/CH–Br foil drives a $\sim 40$ km/s shock inside a gas cell filled with argon at an initial pressure of 1 bar. The use of gas-cell targets with large (several millimetres) lateral and axial extent allows the shock to propagate freely without any wall interactions, and permits a large field of view to image single and colliding counter-propagating shocks with time-resolved, point-projection X-ray backlighting ($\sim 20$ μm source size, 4.3 keV photon energy). Single shocks were imaged up to 100 ns after the onset of the laser drive, allowing to probe the growth of spatial nonuniformities in the shock apex. These results are compared with experiments looking at counter-propagating shocks, showing a symmetric drive that leads to a collision and stagnation from $\sim 40$ ns onward. We present a preliminary comparison with numerical simulations with the radiation hydrodynamics code ARWEN, which provides expected plasma parameters for the design of future experiments in this facility.

In this paper, we present a reanalysis of the silicon He-$\mathrm{\alpha}$ X-ray spectrum emission in Fujioka et al.’s 2009 photoionization experiment. The computations were performed with our radiative-collisional code, RCF. The central ingredients of our computations are accurate atomic data, inclusion of satellite lines from doubly excited states and accounting for the reabsorption of the emitted photons on their way to the spectrometer. With all these elements included, the simulated spectrum turns out to be in good agreement with the experimental spectrum.

Magnetic reconnection driven by laser plasma interactions attracts great interests in the recent decades. Motivated by the rapid development of the laser technology, the ultra strong magnetic field generated by the laser-plasma accelerated electrons provides unique environment to investigate the relativistic magnetic field annihilation and reconnection. It opens a new way for understanding relativistic regimes of fast magnetic field dissipation particularly in space plasmas, where the large scale magnetic field energy is converted to the energy of the nonthermal charged particles. Here we review the recent results in relativistic magnetic reconnection based on the laser and collisionless plasma interactions. The basic mechanism and the theoretical model are discussed. Several proposed experimental setups for relativistic reconnection research are presented.

实验室天体物理是交叉于高能量密度等离子体物理学与天体物理学之间的一个新的学科生长点。利用强激光装置可以在实验室创造与某些天体或天体周围相似的极端物理环境，这样的实验条件前所未有，且与天体物理中诸多重要的物理现象直接对应。通过近距、主动、参数可控的研究，实验室天体物理有助于解决目前天体物理和等离子体物理中的一些关键的、共性的问题，并有望取得突破性成果。针对近年来国内外在该领域取得的最新研究进展进行介绍，并就将来可能开展的研究方向进行展望。

A developing application of laser-driven currents is the generation of magnetic fields of picosecond–nanosecond duration with magnitudes exceeding $B=10~\text{T}$. Single-loop and helical coil targets can direct laser-driven discharge currents along wires to generate spatially uniform, quasi-static magnetic fields on the millimetre scale. Here, we present proton deflectometry across two axes of a single-loop coil ranging from 1 to 2 mm in diameter. Comparison with proton tracking simulations shows that measured magnetic fields are the result of kiloampere currents in the coil and electric charges distributed around the coil target. Using this dual-axis platform for proton deflectometry, robust measurements can be made of the evolution of magnetic fields in a capacitor coil target.

Space debris laser ranging was achieved with a 60 W, 200 Hz, 532 nm nanosecond slab, single-frequency green laser at the Shanghai Astronomical Observatory’s 60 cm satellite laser ranging system. There were 174 passes of space debris measured in 2017, with the minimum radar cross section (RCS) being 0.25 m² and the highest ranging precision up to 13.6 cm. The RCS of space debris measured with the farthest distances in 174 passes was analyzed. The results show that the farthest measurement distance (R) and RCS (S) were fitted to R = 1388.159S^0.24312, indicating that this laser can measure the distance of 1388.159 km at an RCS of 1 m², which is very helpful to surveillance and research on low-Earth-orbit space debris.

This paper describes a model of electron energization and cyclotron-maser emission applicable to astrophysical magnetized collisionless shocks. It is motivated by the work of Begelman, Ergun and Rees [Astrophys. J. 625, 51 (2005)] who argued that the cyclotron-maser instability occurs in localized magnetized collisionless shocks such as those expected in blazar jets. We report on recent research carried out to investigate electron acceleration at collisionless shocks and maser radiation associated with the accelerated electrons. We describe how electrons accelerated by lower-hybrid waves at collisionless shocks generate cyclotron-maser radiation when the accelerated electrons move into regions of stronger magnetic fields. The electrons are accelerated along the magnetic field and magnetically compressed leading to the formation of an electron velocity distribution having a horseshoe shape due to conservation of the electron magnetic moment. Under certain conditions the horseshoe electron velocity distribution function is unstable to the cyclotron-maser instability [Bingham and Cairns, Phys. Plasmas 7, 3089 (2000); Melrose, Rev. Mod. Plasma Phys. 1, 5 (2017)].