日冕物质抛射引起地磁扰动的分类预报

对1997—2003年期间引起地磁扰动的72个加速日冕物质抛射(CME)事件和69个减速CME事件进行了特性分析，并针对经行星际闪烁(IPS)认证的32个加速CME引起的地磁扰动事件和32个减速CME引起的地磁扰动事件分类建立了新的从属函数μ_T和新的磁扰开始时间修正项, 经验证预报效果得到显著提高.对于加速CME引起的地磁扰动事件，磁扰开始时间的预报值T_pre与观测值T_obs比较，相对误差ΔT_pre/T_obs≤10%的事件占总事件数的21.86%；ΔT_pre/T_obs≤30%的事件为78.13%；而ΔT_pre/T_obs>50%的事件为9.36%；对于减速CME引起的地磁扰动事件相对误差ΔT_pre/T_obs≤10%的事件占总事件数的25.00%；ΔT_pre/T_obs≤30%的事件为84.37%；而ΔT_pre/T_obs>50%的事件仅为3.13%.这表明该预报方法对空间灾害性事件的磁扰动的定量预报具有很大的现实可能性. 关键词： 日冕物质抛射 地磁扰动 从属函数     

行星际日冕物质抛射引起福布斯下降的一维随机微分模拟

福布斯下降(Forbush decrease,FD)是银河宇宙线(galactic cosmic rays,GCRs)受短期剧烈太阳活动调制的重要现象之一.本文设GCRs进入由行星际日冕物质抛射(interplanetary coronal mass ejection,ICME)及其前沿激波共同形成的扰动区时,其径向扩散系数κ_(rr)受抑制变为μ(r)·κ_(rr)(0μ(r)1),且抑制强度与粒子位置处的太阳风等离子体速度正相关.对任意时刻的扰动区,抑制系数μ(r)在激波处最小为μ(r_(sh)),并按指数规律增大,在ICME尾部归一.CME爆发时,μ(r_(sh))取全局最小值μm.在扰动区向日球层外传播的过程中,μ(r_(sh))逐步恢复为1.在此基础上,根据GOES和ACE卫星观测确定模型参数,用一维随机微分方程描述GCRs在日球层内的传播,并采用倒向随机方法模拟了一个由独立Halo ICME调制GCRs引起的2005年5月15日FD事件.计算所得地面中子通量的主相、恢复相及其在CME到达地球前的增加过程,均与Oulu中子探测器观测结果一致.     

一种耦合外部电路的脉冲感应推力器磁流体力学数值仿真模型

为了深入研究脉冲感应推力器的工作原理,预测其推进性能,建立了一种耦合外部电路的磁流体力学模型,实现了对加速通道内等离子体二维流场结构演化过程及驱动电路放电过程的同步耦合求解.模拟计算所得美国MK-1推力器加速通道内的等离子体瞬态参数分布及推力器比冲、效率等性能参数均与实验数据一致;计算结果成功复现了推力器的工作物理图景.借助这一新模型,实现了对电路-等离子体双向耦合作用的定量分析,分析结果表明:耦合等离子体导致驱动电路等效电阻增大,电感减小;激励线圈与等离子体之间的互感随等离子体整体远离线圈表面而逐渐减小.     

FP-1装置铝套筒内爆动力学过程的一维磁流体力学模拟

作为一种重要的柱面会聚冲击和准等熵压缩加载源,磁驱动固体套筒内爆技术已广泛应用于高能量密度物理实验研究.针对FP-1装置驱动的固体套筒内爆动力学过程,建立了含强度的一维磁流体力学模型,并对典型实验进行了模拟.计算获得的套筒内爆速度同实验结果较为相符.模拟结果显示,该装置在40 kV充压条件下,可以将直径3 cm,厚0.5 mm的铝套筒加速至1.1 km/s,内壁速度超过1.5 km/s,同时保持大部分材料为固体状态.内爆套筒与相同材料靶筒碰撞产生的冲击压力约9 GPa.改变靶筒内部填充气体的压力,可以获得不同的靶筒运动速度、轨迹以及反弹半径,以满足不同类型实验的研究需要.     

等离子体断路开关的一维磁流体力学数值模拟

 采用磁流体力学的方法对等离子体端路开关进行了一维数值模拟，通过对给定的进入等离子体的电流波形模型的计算，给出了轴向上等离子体的运动及其不同时刻的密度分布，分析了磁场在等离子体内部的异常渗透过程，指出考虑Hall效应是产生这一异常现象的最为主要的因素。     

内爆圆柱套筒磁通量压缩的磁流体力学计算

在一维反应流体动力学程序SSS的基础上扩充编制一维磁流体力学计算编码SSS/MHD,并对炸药内爆驱动的圆柱形套筒磁通量聚积发生器（MC-1装置）进行了一维磁流体力学模拟计算。分析了空腔磁场向压缩套筒和样品套筒壁中的磁扩散现象,结果表明,在压缩套筒壁中距离空腔0.2 mm处的磁感应强度最大值只有十几T;而在样品套筒壁中距离空腔0.2 mm处的磁感应强度最大值达到几百T,这主要是内外套筒运动速度不同,电磁力与内爆作用力平衡引起的。计算了空腔中磁感应强度的变化曲线和样品套筒内壁的速度历程曲线,得到与实验测试符合的结果。     

内爆圆柱套筒磁通量压缩的磁流体力学计算

在一维反应流体动力学程序SSS的基础上扩充编制一维磁流体力学计算编码SSS/MHD,并对炸药内爆驱动的圆柱形套筒磁通量聚积发生器(MC-1装置)进行了一维磁流体力学模拟计算。分析了空腔磁场向压缩套筒和样品套筒壁中的磁扩散现象,结果表明,在压缩套筒壁中距离空腔0.2mm处的磁感应强度最大值只有十几T;而在样品套筒壁中距离空腔0.2mm处的磁感应强度最大值达到几百T,这主要是内外套筒运动速度不同,电磁力与内爆作用力平衡引起的。计算了空腔中磁感应强度的变化曲线和样品套筒内壁的速度历程曲线,得到与实验测试符合的结果。     

含气泡液态金属的磁流体力学和Hartmann流动

本文给出含气泡液态金属的磁流体力学基本方程,以及Hartmann流动的解。     

赤道面磁层顶位形的磁流体力学模拟研究

磁层顶位置和形状的动态特征描绘是地球物理和空间物理研究的难点之一.文章基于太阳风-磁层-电离层耦合的全球磁流体力学（MHD）数值模拟,运用电流密度极大法确定磁层顶位形,并具体研究两种典型太阳风动压（D_p）和几种不同行星际磁场的z分量（B_z）条件下,地球赤道面上方磁层顶动态特征.模拟结果显示,磁层顶日下点高度r₀主要由D_p控制.随着D_p增加,磁层顶被压缩,r₀显著减小.相同D_p条件下,在B_z由南向（B_z<0）逐渐减小,并转为北向（B_z>0）逐渐增大的过程中,r₀缓慢增大.不同条件下,磁层项张角φ变化较小,反映了赤道面磁层顶结构的相似性.与Shue98低纬磁层顶经验模型比较,MHD模拟能再现磁层顶日下点位置r₀对D_p的响应,而r₀随B_z变化的饱和性仅出现在低速太阳风条件下.MHD模拟和经验模型的磁层项张角φ差别小于2.5°,但模拟显示φ随B_z的变化趋势并非简单线性关系.     

MFCG 2维磁流体力学程序中磁场计算的改进

定子线圈中的电流在空间中产生的磁场是金属导体（套筒）膨胀压缩的主要对象,该磁场直接影响爆磁压缩发生器输出电流脉冲的大小。给出了面电流分布下2维磁场的计算公式,较点电流分布下的磁场公式更能细致准确地反映出磁场的变化。数值结果表明:面电流分布下的磁场公式不仅能准确地描述磁场的变化,而且计算效率大大提高,节约了计算时间。     

Modulation of galactic cosmic ray intensities by coronal mass ejections into interplanetary space

The data on the measurements of the intensities of galactic cosmic rays with proton energies greater than 30 MeV are compared with the data on the solar wind and interplanetary magnetic field measured on board the Vega-1 and Vega-2 automated interplanetary stations. Modulation structures with characteristic shapes and durations, namely quasi-symmetric (“bays”) short-term Forbush decreases of intensity, are revealed. It is shown that these Forbush decreases were recorded due to the stations flying through coronal mass-ejection regions. Original Russian Text ? E.A. Chuchkov, V.I. Tulupov, V.P. Okhlopkov, G.P. Lyubimov, 2009, published in Vestnik Moskovskogo Universiteta. Fizika, 2009, No. 3, pp. 90–93.     

Proton spectrum of the 2005 January 20 solar flare

An extreme solar cosmic ray event broke out on 2005 January 20. Not only is it the most intensive solar energetic particle (SEP) event, with >100MeV particles measured by GOES satellite since 1986, but it has been the largest ground level enhancement (GLE) event recorded by the ground-based neutron monitors since 1956. This work presents the solar proton spectra for this event with data obtained by GOES in multiple energy channels. These spectra are well fitted by a modified power-law function. The spectral index of around －1 indicates that the January 20 event has a hard energy spectrum. Possible mechanisms for the acceleration of relativistic protons are discussed.     

Eruptive events in the solar atmosphere: new insights from theory and 3-D numerical modelling

Ejections of magnetised plasma from the Sun, commonly known as coronal mass ejections (CMEs), are one of the most stunning manifestations of solar activity. These ejections play a leading role in the Sun–Earth connection, because of their large-scale, energetics and direct impact on the space environment near the Earth. As CMEs evolve in the solar corona and interplanetary space they drive shock waves, which act as powerful accelerators of charged particles in the inner solar system. Some of these particles, known as solar energetic particles (SEPs), can strike our planet, and in doing so they can disrupt satellites and knock out power systems on the ground, among other effects. These particles, along with the intensive X-ray radiation from solar flares, also endanger human life in outer space. That is why it is important for space scientists to understand and predict the ever changing environmental conditions in outer space due to solar eruptive events – the so-called space weather. To enable the development of accurate space weather forecast, in the past three decades solar scientists have been challenged to provide an improved understanding of the physical causes of the CME phenomenon and its numerous effects. This paper summarises the most recent advances from theory and modelling in understanding the origin and evolution of solar eruptive events and related phenomena.     

Effect of solar features and interplanetary parameters on geomagnetosphere during solar cycle-23

The dependence of geomagnetic activity on solar features and interplanetary (IP) parameters is investigated. Sixty-seven intense (−200 nT ≤ Dst < −100 nT) and seventeen superintense (Dst < −200 nT) geomagnetic storms (GMSs) have been studied from January 1996 to April 2006. The number of intense and superintense GMSs show three distinct peaks during the 11-year period of 23rd solar cycle. The largest number of high strength GMSs are observed during maximum phase of solar cycle. Halo and partial halo CMEs are likely to be the major cause for these GMSs of high intensity. No relationship is observed between storm duration and the number of CMEs involved in its occurrence. The intensity of the GMS is also independent of the number of CMEs causing the occurrence of storm. These geoeffective CMEs show western and northern bias. Majority of the geoeffective CMEs are associated with X-ray solar flares (SFs). Solar and IP parameters, e.g., V _CME, V _SW, B, B _z (GSE and GSM coordinates) and their products, e.g., V _SW · B and V _SW · B _z are observed and correlated to predict the occurrence of intense GMSs. V _CME does not seem to be the appropriate parameter with the correlation coefficient, r = −0.2 with Dst index, whereas the correlation coefficient, r = −0.57, −0.65, 0.75, −0.68 and 0.77 of the parameters V _SW, B, B _z , V _SW · B and V _SW · B _z respectively, with Dst indicating that V _SW · B _z and B _z may be treated as the significant contributors in determining the strength of GMSs.      

太阳爆发：源动力之谜

看似宁静的太阳上存在着诸多活动现象,其中的爆发活动,包括耀斑(solar flares)和日冕物质抛射(CMEs),是太阳系内最剧烈的能量释放,也是造成空间环境和空间天气变化的最主要因素。磁场重联一直被认为是其背后的驱动力,然而确凿的证据一直没有找到。现在,新一代观测卫星太阳动力学天文台(SDO)终于记录到了完整可信的日冕重联过程。文章中我们简要回顾太阳爆发的研究历史,介绍最新的研究成果,并讨论将来的研究重点。     

Study of solar features causing GMSs with 250γ<<Emphasis Type="Italic">H</Emphasis><400γ

The effect of solar features on geospheric conditions leading to geomagnetic storms (GMSs) with planetary index,A ^P ≥ 20 and the range of horizontal component of the Earth’s magnetic fieldH such that 250γ <H < 400γ has been investigated using interplanetary magnetic field (IMF), solar wind plasma (SWP) and solar geophysical data (SGD) during the period 1978–99. Statistically, it is observed that maximum number of GMSs have occurred during the maximum solar activity years of 21st and 22nd solar cycles. A peculiar result has been observed during the years 1982, 1994 when sunspot numbers (SSNs) decrease very rapidly while numbers of GMSs increase. No distinct association between yearly occurrence of disturbed days and SSNs is observed. Maximum number of disturbed days have occurred during spring and rainy seasons showing a seasonal variation of disturbed days. No significant correlation between magnitude (intensity) of GMSs and importance ofH _α , X-ray solar flares has been observed. Maximum number of GMSs is associated with solar flares of lower importance, i.e., SF during the period 1978-93.H _α , X-ray solar flares occurred within lower helio-latitudes, i.e., (0–30)°N to (0–30)°S are associated with GMSs. NoH _α , X-ray solar flares have occurred beyond 40°N or 40°S in association with GMSs. In helio-latitude range (10–40)°N to (10–40)°S, the 89.5% concentration of active prominences and disappearing filaments (APDFs) are associated with GMSs. Maximum number of GMSs are associated with solar flares. Coronal mass ejections (CMEs) are related with eruptive prominences, solar flares, type IV radio burst and they occur at low helio-latitude. It is observed that CMEs related GMS events are not always associated with high speed solar wind streams (HSSWSs). In many individual events, the travel time between the explosion on the Sun and maximum activity lies between 58 and 118 h causing GMSs at the Earth.     

On ejection of solar plasma enriched with 3He and Fe I at boundaries of coronal holes

The spectra and spectroheliograms in the He I λ = 1083.03 nm IR-line obtained with the horizontal solar telescope of the Sternberg State Astronomical Institute (SSAI) of Moscow State University are analyzed for the purpose of studying the increased solar activity at the boundaries of coronal holes. Our observations demonstrate plasma flux intensification at the boundary separating a coronal hole and a bipolar active region. In this case, the spectra in the vicinity of the He I λ = 1083.03 nm line point to a significant intensification in the lines of light isotope ³He I λ = 1083.168 nm and Fe I λ = 1082.837 nm. Acceleration of solar plasma fluxes at the coronal hole boundary in the immediate vicinity of an active region seems to be the result of reconnection of bipolar structure magnetic fields in the active region and a unipolar field of the coronal hole. The nature of ³He and Fe I particle enrichment in upward fluxes at the coronal hole boundaries is discussed. Original Russian Text ? L.M. Kozlova, B.V. Somov, 2009, published in Vestnik Moskovskogo Universiteta. Fizika, 2009, No. 3, pp. 94–98.     

Z箍缩丝阵烧蚀的简单模型数值模拟

丝阵烧蚀在丝阵Z箍缩动力学中扮有重要角色,透彻理解丝阵烧蚀对于丝阵Z箍缩动力学的研究至关重要。采用简单模型数值模拟了烧蚀过程,该模型物理上采用绝热、单流体、单相、磁流体力学近似,数值上采用欧拉法结合保单调输运格式来离散。数值结果很好地展示了烧蚀过程的主要特征,例如芯-冕结构、径向等离子体流、轴线上先驱等离子体柱的形成、静止丝芯的长寿命以及延长的烧蚀期,一些关键时间参数定量或定性地相符于文献报道的实验和数值结果,例如冕等离子体角向融合的时刻、等离子体首次到达轴线的时刻、丝芯静止持续的时间、最后的箍缩滞止时刻,但某些方面略有差异。