Introduction of laboratory astrophysics with intense lasers
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摘要: 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。Abstract: Laboratory astrophysics came into being with the advent of modern high-energy density physics research devices that can be used to create extreme physical conditions in the laboratory similar to those of certain celestial bodies or their surroundings, such as high-power lasers or pinch devices to generate extreme astrophysical plasma conditions. Such experimental conditions are unprecedented and correspond directly to many important and critical physical phenomena in astrophysics. They enable people to study the problems with astrophysical background in the laboratory in a close, active and controllable way. This paper introduces the latest progress in this field in recent years, and presents perspectives on future research directions.
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Key words:
- laboratory astrophysics /
- intense lasers /
- magnetic reconnection /
- opacity /
- jet
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图 1 （a）双模造父变星的前两个谐波周期的比值与恒星质量的关系。黑色圆圈表示观测值。黑色虚线为Cox 和 Tabor[13]使用旧的不透明度计算得到的周期。黑色实线为使用实验标定后OPAL-DTA模型得到的周期。M☉是太阳质量，P0是基模周期，P1是第一谐变周期。（b）Bailey等人实验的布置图[25]。（c）Bailey等人实验中得到的空间和光谱分辨的透过率的图。暗色的区域对应于高吸收，白色区域对应于100%的透过率[25]
Figure 1. （a）Diagram of the ratio of the first two harmonics periods of double-mode Cepheid variable star. Circles represent observations. The upper set of three （dashed） curves correspond to the simulated result using older opacities，which ignore the full fine structure of the metals and calculated by Cox and Tabor[13]. The lower （solid） curves correspond to simulations with OPAL-DTA. M☉ is the solar mass，P0 is the fundamental mode period and P1 is the first overtone period. （b） Experimental setup of Bailey et al 2015[25]. （c） A spatially resolved and spectrally resolved transmission image obtained by Bailey et al 2015. Darker regions correspond to higher absorption. The white portion of the image corresponds to 100% transmission[25].
图 6 （a）磁场分布以及环顶X射线源的示意图。（b）靶前的针孔相机拍摄的X射线结果。（c）不对称激光强度导致激光光斑以及磁场B1和B2的不平衡的X射线结果[5]
Figure 6. （a） Magnetic reconnection model for the loop-top X-ray source in a compact solar flare，with a sketch depicting the X-ray observation scheme. （b） The pinhole X-ray image observed forward of the Al foil target. （c） The pinhole X-ray result of unbalanced laser intensity leading to laser spot and unbalanced magnetic fields B1 and B2[5]
图 12 （a）无外加磁场为零，（b）外加磁场是0.4 T。（a）和（b）是实验中阴影图的图像，（c）和（d）是对比增强数据，（e）～（h）表示外加0.4 T磁场时，在不同时刻，KHI演化区域的磁场分布图[73]
Figure 12. （a） The magnetic field of a magnet was null. （b） the magnetic field was 0.4 T. （a） and （b） are images from the shadowgraphs in the experiments，and （c） and （d） are contrast-enhanced data. （e）～（h） The distribution of magnetic field in the evolution region of KHI during 0～9 ns[73]
图 17 脉冲型太阳耀斑能谱及实验室耀斑实验电子能谱
Figure 17. Energy spectrum of pulsed solar flare and electron energy spectra of laboratory flare experiments
research topic same physics similar physics relative physics laser plasma interaction collision between molecular clouds particle transport non-local transport of neutrino in young neutron star hydrodynamics and shocks equation of state （giant planet） interaction of molecular cloud with strong shock wave generated in supernovae remnant：solar flare，solar wind in solar-terrestrial space，generation and collimation of jet collisionless shock and particle acceleration （origin of cosmic rays） hydrodynamics instabilities generation and amplification of magnetic field Rayleigh-Taylor instability during supernovae explosion；Kelvin-Helmholtz instability during the interaction between solar wind and earth’s magnetic field hydrodynamics instabilities during neutrino driven supernovae explosion；Rayleigh-Taylor instability in planetary nebula atomic physics and X-ray transport opacity （stellar evolution） non-local thermodynamic equilibrium （non-LTE） plasma spectroscopy non-LTE atomic physics in supernovae remnant；stellar jets （non-relativistic） radiation hydrodynamics in early galaxy；photoionized plasma X-ray laser in the universe laser-produced relativistic plasma fireball model of gamma-ray bursts；cosmological jets 
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length/cm time/s pressure/Pa density/cm−3 velocity/（km·s−1） magnetic field/T flare plasmas 109 ～ 1010 100 ～ 1000 0.001 ～ 10 109 ～ 1011 10 ～ 100 10−3 ～ 10−2 laser-produced plasmas ～10−1 ～10−9 ～107 1019 ～ 1020 ～100 ～102 flare plasmas （scaled） 10−2～ 10−1 10−10 ～10−9 107 ～ 1011 1019 ～ 1021 100 ～ 1000 102 ～ 103
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表 3 光致电离等离子体中重要的原子过程
Table 3. Atomic transitions in photoionized plasmas
direct process inverse process radiative decay（A） photoexcitation（PE） photoionization（PI） radiative recombination（RR） collisional excitation（CE） collisional deexcitation（CD） collisional ionization（CI） three-body recombination（TR） autoionization（AI） dielectronic capture（DC）
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