激光等离子体强磁环境研究进展

高功率强激光技术的发展使得在实验室模拟复杂天体等离子体环境成为可能。近年来在激光等离子体强磁环境下模拟天体物理现象是实验室天体物理研究的一个热点方向,文章简单介绍了利用强激光产生强磁场的各种机制,包括毕尔曼电池效应、线圈靶诱发磁场等,并介绍了在实验室诊断此类磁场的一些常用方法,如法拉第旋转法、质子背光法、B-dot法等。最后介绍该方向几个研究的最新进展,包括磁场压缩、喷流等,同时提出一些在实验室产生强磁场的新思路。     

磁场对激光驱动的喷流演化影响的二维数值研究

喷流的触发机制、准直传输和稳定性一直是天体物理学的研究热点.近年通过观测和实验室研究发现磁场在喷流准直传输和加速中起着关键作用.本文利用开源的辐射磁流体模拟程序FLASH对强激光驱动聚苯乙烯(CH)平面靶产生的靶前喷流进行了二维的数值模拟,系统地考察和比较了Biermann自生磁场以及不同方向、不同初始强度的外加磁场对喷流演化的动力学.模拟结果表明Biermann自生磁场不会影响喷流的界面动力学,而外加磁场对等离子体出流具有重定向作用,平行于靶前等离子体出流中心流向的外加磁场有助于喷流的产生和准直传输.其形成和演化过程是等离子体热压、磁压以及冲压三者相互竞争的结果.在受力方面,在喷流演化过程中等离子体热压梯度力和磁压力起决定性作用.研究结果为后续开展和喷流相关的实验研究提供借鉴,也有助于加深对天体喷流演化的理解.     

激光加速电子束放射照相的模拟研究

激光加速产生高能量电子束具有源尺寸小、准单能、脉宽窄等特征.通过蒙特卡罗程序模拟研究了高能电子束的放射照相.模拟了200 MeV准直电子束照射台阶靶、厚铁靶,11 MeV点源电子束照射惯性约束聚变模型靶,以及70 MeV点源电子束在激光等离子体磁场下的偏转.结果表明激光加速电子束在探伤厚材料内部、确认薄材料界面、测量电磁场等诊断中具有高时空分辨、灵敏等能力.     

纳秒激光烧蚀固体靶产生的等离子体在外加横向磁场中膨胀时的温度和密度参数演化

利用等离子体光学波段自发光成像、光学光谱和光学探针干涉等诊断手段, 观察了纳秒脉冲激光烧蚀固体靶产生的等离子体在外加横向磁场中的膨胀过程. 根据实验参数特征建立了简化的磁流体物理模型, 结合自发光强度的时间演化, 理论计算了等离子体温度和密度参数的时间演化, 理论计算结果与实验测量结果基本符合, 证实了碰撞磁扩散过程在等离子体演化中发挥了关键作用.     

激光烧蚀Al靶产生的等离子体中辐射粒子的速度及激波

在低真空条件下(5Pa),通过测量脉冲激光烧蚀平面Al靶产生的等离子体辐射谱的时间分辨特征,得到辐射粒子速度的空间分布.在激光脉冲宽度为10ns,烧蚀斑直径为200μm,靶面上功率密度分别为1.91×10¹⁰,5.10×10¹⁰和7.64×10¹⁰W/cm²时,测得辐射粒子Al的速度均在10⁶cm/s量级,且随着靶面径向距离的增大而近似呈指数衰减.在距靶面的相同距离处,激光功率密度的增大反而使速度减小.利用激波模型(shockwave model)较好地解释了实验结果,并得出激波的波面基本为柱对称 关键词： 激光等离子体 平面Al靶 粒子速度分布 激波     

强场物理中自生磁场的实验研究

为了获得飞秒激光与固体靶相互作用中自生磁场的大小与空间分布情况, 利用光学多道分析（OMA）谱仪（谱分辨0.1nm ）加电荷耦合器件（CCD）相机（11521242）探测设备, 用消色差的相机镜头作为空间分辨,在固体靶前表面测量了激光的高次谐波（n0）光谱, 观测到了n0光谱的精细结构及其频率间隔,由此推出激光与固体靶相互作用中产生的等离子体内的自生磁场达60-70特斯拉（T）量级, 且越接近靶法线方向磁场越强,其一维空间分布为环形。 这一结果为进一步研究强场物理中自生磁场的特性及等离子体的整体行为提供了依据。     

次稠密等离子体对激光与锥形靶相互作用的影响

利用三维粒子模拟程序模拟了强激光在锥形靶内的传播情况.发现锥内次稠密等离子体的存在使激光在锥顶部的最大聚焦强度有所降低，产生的相对论电子的最大能量和数目增加.激光在锥壁激发起强的电流和磁场，次稠密的存在还使锥内产生强的准静态磁场，磁场的存在使相对论电子速度分布在垂直激光传播方向上表现出各向同性. 关键词： 超强激光脉冲 锥形靶 快点火 粒子模拟     

用于激光等离子体中脉冲强磁场产生的电感耦合线圈

脉冲强磁场装置是磁化激光等离子体实验的核心设备.本文研制了一种用于优化脉冲强磁场设备的电感耦合线圈,相对于单匝磁场线圈可以进一步提高磁场强度.通过实验和模拟研究了电感耦合线圈的初级螺线管匝数和直径对磁场强度的影响,发现对于2.4μF电容的放电系统,电感耦合线圈的初级螺线管在35匝、35 mm直径时,可以在5 mm内径的次级磁场线圈中获得最高的峰值磁场强度,是相同尺寸单匝磁场线圈产生磁场强度的3.6倍.在充电电压20 kV时,峰值磁场强度达到19 T,使用铍铜材料的电感耦合线圈克服强磁场中线圈炸裂问题,在35 kV的充电电压下得到了33 T的峰值磁场强度.这种新方法产生了更强的磁场、降低了对回路电感的要求、提升了实验排布的灵活性,为研究强磁场下的激光等离子体行为创造了条件.     

超高速碰撞产生磁场的1维模型

 为研究超高速弹丸碰撞靶板产生等离子体诱生的磁场,引用已有关于激光产生等离子体的磁场理论,结合麦克斯韦方程和法拉第电磁感应定律得到了超高速碰撞产生等离子体诱生磁场的1维理论模型。基于已有关于超高速正碰撞产生半球状等离子体云诱生磁场的偏微分方程,建立了柱坐标系下超高速斜碰撞产生部分椭球状等离子体云的偏微分方程。通过感应线圈进行了磁感应强度的实验测量,实验结果与模型预言表明,该模型可近似地描述超高速斜碰撞产生等离子体诱生的磁感应强度。     

一种脉冲强电流条件下导线电阻测量方法

在超强激光辐照电容线圈靶产生强磁场实验中,在约50 ps时,线圈电流达到20 kA以上。通过该实验结果与磁场产生理论模型对比,可得出该导线电阻值比常温直流电阻高出3个量级。对导线材料电阻率与趋肤效应的分析结果表明,该电阻值在量级上是合理的。获得超快脉冲强电流条件下的导线电阻值,有助于更深入理解线圈靶产生强磁场过程。     

Promising lines of investigations in the realms of laboratory astrophysics with the aid of powerful lasers

The results of work on choosing and substantiating promising lines of research in the realms of laboratory astrophysics with the aid of powerful lasers are presented. These lines of research are determined by the possibility of simulating, under laboratory conditions, problematic processes of presentday astrophysics, such as (i) the generation and evolution of electromagnetic fields in cosmic space and the role of magnetic fields there at various spatial scales; (ii) the mechanisms of formation and evolution of cosmic gamma-ray bursts and relativistic jets; (iii) plasma instabilities in cosmic space and astrophysical objects, plasma jets, and shock waves; (iv) supernova explosions and mechanisms of the explosion of supernovae featuring a collapsing core; (v) nuclear processes in astrophysical objects; (vi) cosmic rays and mechanisms of their production and acceleration to high energies; and (vii) astrophysical sources of x-ray radiation. It is shown that the use of existing powerful lasers characterized by an intensity in the range of 10¹⁸–10²² W/cm² and a pulse duration of 0.1 to 1 ps and high-energy lasers characterized by an energy in excess of 1 kJ and a pulse duration of 1 to 10 ns makes it possible to perform investigations in laboratory astrophysics along all of the chosen promising lines. The results obtained by experimentally investigating laser plasma with the aid of the laser facility created at Central Research Institute of Machine Building (TsNIIMash) and characterized by a power level of 10 TW demonstrate the potential of such facilities for performing a number of experiments in the realms of laboratory astrophysics.     

强激光天体物理学研究——在强激光实验室中模拟某些天体物理过程(Ⅰ)

用激光等离子体相互作用对天体物理过程进行模拟研究已成为当前世界物理和天文学家深感兴趣的重要前沿领域 .文章比较了强激光作用下产生的等离子体与天体物理条件下的等离子体之间在内部物理过程的相似性 ,论述了由前者模拟后者的物理依据 ,即相似性原则和定标规律 .在此基础上 ,回顾和评述了当前已经在高离化态光谱学、类天体等离子体状态方程和辐射不透明度以及流体动力学不稳定性等方面开展的强激光天体物理学的研究 ,这些研究对于理解超新星、白矮星、中子星以及巨行星、褐矮星等领域的天体物理过程起到了极大的作用 ,并正在成为联系天体物理理论模拟和观测的中间桥梁     

Relativistic laser-matter interaction and relativistic laboratory astrophysics

The paper is devoted to the prospects of using the laser radiation interaction with plasmas in the laboratory relativistic astrophysics context. We discuss the dimensionless parameters characterizing the processes in the laser and astrophysical plasmas and emphisize a similarity between the laser and astrophysical plasmas in the ultrarelativistic energy limit. In particular, we address basic mechanisms of the charged particle acceleration, the collisionless shock wave and magnetic reconnection and vortex dynamics properties relevant to the problem of ultrarelativistic particle acceleration.     

强激光天体物理学研究

用激光等离子体相互作用对天体物理过程进行模拟研究已成为当前世界物理和天文学家深感兴趣的重要前沿领域.文章比较了强激光作用下产生的等离子体与天体物理条件下的等离子体之间在内部物理过程的相似性,论述了由前者模拟后者的物理依据,即相似性原则和定标规律.在此基础上,回顾和评述了当前已经在高离化态光谱学、类天体等离子体状态方程和辐射不透明度以及流体动力学不稳定性等方面开展的强激光天体物理学的研究,这些研究对于理解超新星、白矮星、中子星以及巨行星、褐矮星等领域的天体物理过程起到了极大的作用,并正在成为联系天体物理理论模拟和观测的中间桥梁.     

激光驱动的冲击波自生磁场以及外加磁场的冲击波放大研究

冲击波是天体物理观测中常见的现象, 其对粒子的加速被认为是高能宇宙射线的来源. 宇宙中冲击波周围往往存在很强的磁场, 但人们对于此类强磁场的产生放大过程的理解并不充分. 本文利用二维粒子模拟程序研究了激光与磁化或者非磁化等离子体相互作用产生的冲击波现象, 给出了冲击波波前处磁场的产生放大特性. 研究发现, 作用过程中的自生磁场可以储存能量, 从而进一步加速电子; 当存在外加磁场时, 由冲击波加速的电子和离子的能量都比同条件下非磁化等离子体的能量高; 而且外加磁场藉由冲击波放大倍数则与其值有极大关系. 与天文观测中推断的磁场与背景磁场相比放大千倍这一研究结果的比较可以看出, 天体冲击波周围磁场放大主要是由局域内生磁场导致的.     

Ion-pressure equations derived from measurements in space

Cluster measurements at the bow shock, the magnetosheath, and the magnetospheric boundary layer are used to derive ion-pressure equations for hot anisotropic plasmas. It is demonstrated that both perpendicular and parallel ion pressures are well approximated by polybaric expressions is proportional to N(gamma)B(kappa), where N is the plasma density, B is the magnetic field, gamma is in the range 0.5 to 2, and kappa is between -2 and 0. The parameters derived from observations are distinctively different from those predicted by double-adiabatic theory and are shown to hold for pressure variations over 4 orders of magnitude and for a range of plasma beta (ratio of kinetic/magnetic pressures) between 10(-4) and 10. The results are relevant for simulations and theories of astrophysical, solar, interplanetary, and magnetospheric processes based on MHD equations.     

Simulation of Supernova Expansion

We study the possibility of laboratory modeling of some processes that are intrinsic to supernova (SN) explosion by means of powerful lasers (the so-called laboratory astrophysics); in particular, the possibility of reproducing astrophysical data via numerical models was originally aimed at laser plasma simulation. First of all, we analyze hydrodynamic similarity criteria for the considered processes. Then, we conduct 1D and 2D hydrodynamic simulations to model the expansion dynamics of the SN remnant (the progenitor mass is ～5–15 that of the Sun) during several hundreds of seconds after the explosion, including initially asymmetric configurations. Basing on the similarity criteria, we consider possible laser targets – simulators for a supernova, which mimic some processes inherent in astrophysical phenomenon, such as shock wave propagation through a medium, the development of hydrodynamic instabilities at contact boundaries of shells of different densities, etc. We present a simple solution to the problem of blast wave propagation in a medium with density distributed according to a decreasing power law, which is a good approximation for the density distribution in a supernova progenitor.     

Laser cosmology

Recent years have witnessed tremendous progress in our understanding of the cosmos, which in turn points to even deeper questions to be further addressed. Concurrently the laser technology has undergone dramatic revolutions, providing exciting opportunity for science applications. History has shown that the symbiosis between direct observations and laboratory investigation is instrumental in the progress of astrophysics. We believe that this remains true in cosmology. Current frontier phenomena related to particle astrophysics and cosmology typically involve one or more of the following conditions: (1) extremely high energy events;(2) very high density, high temperature processes; (3) super strong field environments. Laboratory experiments using high intensity lasers can calibrate astrophysical observations, investigate underlying dynamics of astrophysical phenomena, and probe fundamental physics in extreme limits. In this article we give an overview of the exciting prospect of laser cosmology. In particular, we showcase its unique capability of investigating frontier cosmology issues such as cosmic accelerator and quantum gravity.     

Two‐dimensional magnetosonic shock wave propagation in dense electron–positron–ion plasmas

Two‐dimensional (2D) magnetosonic wave propagation in magnetized quantum dissipative plasmas is studied. The plasma system is comprised of inertial ions, inertia‐less electrons, and positrons. The multi‐fluid quantum hydrodynamic model is used, in which quantum statistical and quantum tunnelling effects of electrons and positrons are included. Reductive perturbation analysis is performed to derive the Zabolotskaya–Khokhlov equation for the 2D propagation of a magnetosonic shock wave in a magnetized qauntum plasma. The effects of varying the different plasma parameters such as positron density and magnetic field intensity on the propagation characteristics of magnetosonic shock waves are discussed with non‐relativistic degenerate plasma parameters in astrophysical plasma situations.     

Influence of the solar-wind magnetic field on the magnetosheath turbulence behind the bow shock

The experiment Sura–-WIND (1996–1997) on radio-raying of geodisturbed solar-wind region is interpreted in terms of modern knowledge of an interaction between the magnetized solar wind and the Earth's magnetosphere. Characteristics of the scattered signal at 9 MHz, determined by a plasma turbulence level with scales about 100 km, are statistically related to in situ measurements of solar wind parameters such as plasma density and the orientation and magnitude of the interplanetary magnetic field (IMF) onboard WIND spacecraft. The dependence of the scintillation index of the detected scattered signal, characterising the average turbulence level of the Earth's magnetosheath behind the bow shock, on the IMF orientation and magnitude is revealed. To verify the relation obtained, modern nonlinear correlation techniques based on the theory of artificial neural networks (ANN) are applied. The results obtained using a three-layer ANN with error backpropagation confirm an essential IMF influence on the plasma turbulence in the magnetosheath.