太阳与内日球立体探测卫星计划科学目标建议

面向认知太阳风暴和保障航天安全的国家战略需求,中国近年来提出太阳与内日球立体探测卫星计划,拟适时部署环黄道面的拉格朗日点L3-L4-L5定点卫星星座和脱离黄道面的太阳极轨对偶卫星。通过该卫星计划的初步科学论证分析,建议将其科学目标凝练为太阳磁场、太阳风暴、太阳风,将其应用目标定位于日地空间天气预报,建议配置成像类、粒子类、波场类的综合科学载荷。此外,利用日地空间的三维磁流体数值模拟和计算机图形学的艺术可视化,形象地表达环黄道面卫星“对日凝视”和太阳极轨卫星“鸟瞰全景”的探测概念。中国太阳与内日球立体探测卫星计划将揭示太阳磁场的起源规律及其爆发机理、日地耦合系统的空间天气变化机理,并能够为日地空间天气三维数值建模提供观测数据驱动的初边值条件,必将极大推动空间天气的立体监测、前沿研究、精准预报的一体化进程。

A 3rd Order WENO GLM-MHD Scheme for Magnetic Reconnection

A new numerical scheme of 3rd order Weighted Essentially Non-Oscillatory (WENO) type for 2.5D mixed GLM-MHD in Cartesian coordinates is proposed. The MHD equations are modified by combining the arguments as by Dellar and Dedner et al to couple the divergence constraint with the evolution equations using a Generalized Lagrange Multiplier (GLM). Moreover, the magnetohydrodynamic part of the GLM-MHD system is still in conservation form. Meanwhile, this method is very easy to add to an existing code since the underlying MHD solver does not have to be modified. To show the validation and capacity of its application to MHD problem modelling, interaction between a magnetosonic shock and a denser cloud and magnetic reconnection problems are used to verify this new MHD code. The numerical tests for 2D Orszag and Tang's MHD vortex, interaction between a magnetosonic shock and a denser cloud and magnetic reconnection problems show that the third order WENO MHD solvers are robust and yield reliable results by the new mixed GLM or the mixed EGLM correction here even if it can not be shown that how the divergence errors are transported as well as damped as done for one dimensional ideal MHD by Dedner et al.

时变行星际太阳风模拟及其结果评估

背景太阳风对于地球附近的空间环境有着重要的影响,三维磁流体力学太阳风模型是背景太阳风研究和预报的重要工具.通过太阳光球磁场数据驱动的边界条件,我们发展了一个时变的行星际三维磁流体力学太阳风模型.使用这个模型,我们模拟了2008年全年的行星际背景太阳风,分析了该年太阳风结构全球特征的演化和行星际局地观测与日冕结构间的联系.实现了一套太阳风连续参数和特征结构模拟质量的定量评估方法.对2008年模拟结果的评估表明,模型较好地重现了背景太阳风的大尺度特征.模拟与观测速度间的相关性系数达到了0.6以上,行星际磁场强度与观测吻合得较好,捕获了全部的行星际磁场极性反转和82.76%的流相互作用区,行星际磁场极性反转的误报率仅为6.67%,流相互作用区的误报率仅为11.11%,两种结构的到达时间误差在1天左右.同时,通过综合分析评估结果,我们明确了高速流结构、内边界磁场分布等模型在进一步改进中需要重点注意的问题.

Splitting Based Scheme for Three-dimensional MHD with Dual Time Stepping

A new hybrid numerical scheme of combining an E-CUSP(Energy-Convective Upwind and Split Pressure) method for the fluid part and the Constrained Transport(CT) for the magnetic induction part is proposed.In order to avoid the occurrence of negative pressure in the reconstructed profiles and its updated value,a positivity preserving method is provided.Furthermore,the MHD equations are solved at each physical time step by advancing in pseudo time.The use of dual time stepping is beneficial in the computation since the use of dual time stepping allows the physical time step not to be limited by the corresponding values in the smallest cell and to be selected based on the numerical accuracy criterion.This newly established hybrid scheme combined with positivity preserving method and dual time technique has demonstrated the accurateness and robustness through numerical experiments of benchmark problems such as the 2D Orszag-Tang vortex problem and the3 D shock-cloud interaction problem.

Application of ADER Scheme in MHD Simulation

The Arbitrary accuracy Derivatives Riemann problem method(ADER) scheme is a new high order numerical scheme based on the concept of finite volume integration,and it is very easy to be extended up to any order of space and time accuracy by using a Taylor time expansion at the cell interface position.So far the approach has been applied successfully to flow mechanics problems.Our objective here is to carry out the extension of multidimensional ADER schemes to multidimensional MHD systems of conservation laws by calculating several MHD problems in one and two dimensions: (ⅰ) Brio-Wu shock tube problem,(ⅱ) Dai-Woodward shock tube problem,(ⅲ) Orszag-Tang MHD vortex problem.The numerical results prove that the ADER scheme possesses the ability to solve MHD problem,remains high order accuracy both in space and time,keeps precise in capturing the shock.Meanwhile,the compared tests show that the ADER scheme can restrain the oscillation and obtain the high order non-oscillatory result.

A Prediction Method for △f_0F_(2min) of a Single Station From Interplanetary Parameters Based on Statistical Study

Using 86 CME-interplanetary shock events,the correlation between the peak values of (a) the solar wind parameters(B_z,E_y,P_(dyn)) and the geomagnetic indices(SYM-H,ASY-H,Kp), (b) the coupling functions(Borovsky,Akasofu,Newell) and the geomagnetic indices,(c) the solar wind parameters/coupling functions/geomagnetic indices and the ionospheric parameter(Δf_0F_(2min)), are investigated.The statistical results show that in group(a),B_(z min) and SYM-H_(min) have the best correlation,that in group(b),the best correlation is between the peak values of Akasofu function (A_(min)) and SYM-H_(min),and that in group(c),the best correlation is between K_(pmax) andΔf_0F_(2min). Based on the statistical results,a method for predicting f_0F_2 of a single station is attempted to be set up.The input is modified B_(z min) and the outputs are SYM-H_(min) andΔf_0F_(2min).Then 25 CME-IPS events that caused geomagnetic storms in 1998 and 2009 are used to check the prediction method. The results show that our method can be used to predict SYM-H_(min) andΔf_0F_(2min).

PROGRESS IN HELIOSPHERIC PHYSICS

This is an overview of progresses in heliospheric physics made in China in the period of June, 2000 to May, 2002. The report is focused on theoretical studies,modelling and observational analysis of interplanetary physical phenomena, and consists of five sections: the acceleration and heating of the solar wind, corona structures, coronal mass ejections, magnetic reconnection phenomena, and in terplanetary transient phenomena. The main achievements made recently by Chinese scientists in related areas are simply listed in corresponding sections without any priority, only certain editorial consideration.

背景太阳风数值模拟的熵守恒格式

背景太阳风研究是根据行星际扰动传播情况预测空间天气状况的基础,磁流体(MHD)模拟是背景太阳风研究的重要手段.采用一种新的数值计算方式,利用Ideal GLM-MHD将计算过程中产生的磁场散度以ch的速度向计算区域外传播,从而消去磁场散度;重构部分使用受约束的最小二乘法,将磁场散度作为约束条件添加到重构中,进一步对重构后的磁场梯度进行修正;通量计算采用满足热力学第二定律的熵守恒格式,该格式能够确保在计算过程中熵不增,保证数值稳定.研究结果表明,该方法应用于太阳风数值模拟的求解得到了更加稳定的结果.

子午工程数据资源概述

东半球空间环境地基综合监测子午链项目(简称"子午工程"),是近地空间环境地基监测网络系统,沿东半球东经120°子午线附近和北纬30°附近的15个台站部署了地磁(电)监测设备、常规无线电监测设备、大型无线电监测设备、宇宙线监测设备、光学监测设备和行星际监测设备,连续监测地球表面20-30公里以上直到几百公里的中高层大气、电离层和磁层,以及十几个地球半径以外的行星际空间,获得地磁场、电场、中高层大气的风场、密度、温度、成分,电离层、磁层和行星际太阳风的速度等空间环境参数,共有163个数据集,时间覆盖2010年至今。子午工程的数据,为研究我国上空空间环境特征,空间天气事件的子午链传播,以及地球空间各个圈层之间的耦合过程等提供了重要的数据支持,有力地推动了现有各类地球空间模型的发展,为我国载人航天和探月工程等航天任务等提供了大量的业务数据支撑。

GPU-accelerated computing of three-dimensional solar wind background

High-performance computational models are required to make the real-time or faster than real-time numerical prediction of adverse space weather events and their influence on the geospace environment.The main objective in this article is to explore the application of programmable graphic processing units(GPUs)to the numerical space weather modeling for the study of solar wind background that is a crucial part in the numerical space weather modeling.GPU programming is realized for our Solar-Interplanetary-CESE MHD model(SIP-CESE MHD model)by numerically studying the solar corona/interplanetary solar wind.The global solar wind structures are obtained by the established GPU model with the magnetic field synoptic data as input.Meanwhile,the time-dependent solar surface boundary conditions derived from the method of characteristics and the mass flux limit are incorporated to couple the observation and the three-dimensional(3D)MHD model.The simulated evolution of the global structures for two Carrington rotations 2058 and 2062 is compared with solar observations and solar wind measurements from spacecraft near the Earth.The MHD model is also validated by comparison with the standard potential field source surface(PFSS)model.Comparisons show that the MHD results are in good overall agreement with coronal and interplanetary structures,including the size and distribution of coronal holes,the position and shape of the streamer belts,and the transition of the solar wind speeds and magnetic field polarities.

An asynchronous and parallel time-marching method: Application to three-dimensional MHD simulation of solar wind

An asynchronous and parallel time-marching method for three-dimensional (3D) time-dependent magnetohydrodynamic (MHD) simulation is used for large-scale solar wind simulation. It uses different local time steps in the corona and the heliosphere according to the local Courant-Friedrichs-Levy (CFL) conditions. The solar wind background with observed solar photospheric magnetic field as input is first presented. The simulation time for the background solar wind by using the asynchronous method is <1/6 of that by using the normal synchronous time-marching method with the same computation precision. Then, we choose the coronal mass ejection (CME) event of 13 November, 2003 as a test case. The time-dependent variations of the pressure and the velocity configured from a CME model at the inner boundary are applied to generate transient structures in order to study the dynamical interaction of a CME with the background solar wind flow between 1 and 230 Rs. This time-marching method is very effective in terms of computation time for large-scale 3D time-dependent numerical MHD problem. In this validation study, we find that this 3D MHD model, with the asynchronous and parallel time-marching method, provides a relatively satisfactory comparison with the ACE spacecraft obser- vations at L1 point.

Predicting the shock arrival time using 1D-HD solar wind model

A 1D-HD shock propagation model is established to predict the arrival time of interplanetary shocks at 1 AU. Applying this model to 68 solar events during the period of February 1997 to October 2000, it is found that our model could be practically equivalent to the STOA, ISPM and HAFv.2 models in forecasting the shock arrival time. The absolute error in the transit time from our model is not larger than those of the other three models for the same sample events. Also, the prediction test shows that the relative error of our model is ≤10% for 31% of all events, ≤30% for 75%, and ≤50% for 84%, which is comparable to the relative errors of the other mod- els. These results might demonstrate a potential capability of our model in terms of real-time forecasting.

Responses of the magnetotail plasma sheet to two interplanetary shocks:TC-1 observations

Two interplanetary shocks are examined to determine the responses of the magnetic field and plasma in the plasma sheet upon the shock impacts by using TC-1 observational data.The two shocks are observed by WIND on November 7,2004.Prior to and after the shock,the IMF is either weakly southward or northward.The responses of the plasma sheet to the two shocks are intense and much similar.When the shock interacts with the magnetosphere,the magnetic field impulsively increases 1-2 min after the geomagnetic field sudden impulse (SI) judged from the Sym-H index change,and the magnetic field line is stretched.On the other hand,all of the ion density,the ion temperature,and the velocity of ion flow in the plasma sheet increase.Interestingly,quasi-periodical oscillations of the ion flow are suddenly enhanced,and the plasma flow is basically perpendicular to the local magnetic field.The responses of the magnetic field and the plasma are nearly simultaneous.The responses in the plasma sheet are probably caused by the lateral compression due to the dynamic pressure enhancement downstream the shock when the shock propagates antisunward in the magnetosheath.

Observations of the field-aligned residual flow inside magnetic cloud structure

In this paper,we report two MC events observed by WIND spacecraft with good examples of fieldaligned residual flow inside the MC structure. For both events,the co-moving frames are determined through the deHoffman-Teller (HT) analysis and the axial orientations are inferred by the newly developed minimal residue (MR) method. The nature coordinate system for both events are constructed with velocity of the HT frame and the inferred MC axis,the field and flow remaining in the HT frame are analyzed at this coordinate system. As a result,we find that the residual flows in the co-moving HT frame of the two MC events are almost anti-parallel to the helical magnetic field. We speculate that the field-aligned residual flows are large scale coherent hydrodynamic vortices co-moving with the MCs at the supersonic speed near 1 AU. Data analyses show that the event in slow ambient solar wind is expanding at 1 AU and another one in fast solar wind does not show apparent expansion. Proton behaviors for both events are quasi-isothermal. Accelerated HT analysis shows that both events have no suitable HT frame with constant accelerations,which suggests that both events may be moving at the constant speed near 1 AU under the assumptions of the HT analysis. For both events,the ratio of the dynamic pressure to the magnetic pressure is larger than that of the thermal pressure to magnetic pressure,which suggests that the dynamic effects due to the plasma flows remaining in the co-moving HT frame are more important than the thermal effects in the study of MC evolution and propagation.

An improved CESE method and its application to steady-state coronal structure simulation

This paper presents an improved space-time conservation element and solution element(CESE)method by applying a non-staggered space-time mesh system and simply improving the calculation of flow variables and applies it to magnetohydrodynamics(MHD)equations.The improved CESE method can improve the solution quality even with a large disparity in the Courant number(CFL)when using a fixed global marching time.Moreover,for a small CFL(say<0.1),the method can significantly reduce the numerical dissipation and retain the solution quality,which are verified by two benchmark problems.And meanwhile,comparison with the original CESE scheme shows better resolution of the improved scheme results.Finally,we demonstrate its validation through the application of this method in three-dimensional coronal dynamical structure with dipole magnetic fields and measured solar surface magnetic fields as the initial input.

WIND observations of plasma waves inside the magnetic cloud boundary layers

Based on the WIND observational data for the plasma waves from thermal noise receptor (TNR) working on the frequency 4―256 kHz and the solar wind and the magnetic fields, we analyze the plasma wave activities in the 60 magnetic cloud’s boundary layers (BLs) and find that there are often various plasma wave activities in the BLs, which are different from those in the adjacent solar wind (SW) and the magnetic clouds (MC). The basic characteris-tics are that: (1) the enhancement of the Langmuir wave near the electronic plasma frequency (fpe) is a dominant wave ac-tivity, which occupies 75% investigated samples; (2) the events enhanced both in the langmuir and ion acustic (f < fpe) waves are about 60% of investigated samples; (3) broadband, continuous enhancement events in the plasma wave activities were observed in the whole frequency band of TNR, and about 30% of the 60 samples, however, were not observed in the SW and the MC investigated events; (4) although the ratio of the temperatures between the electon and proton, Te/Tp≤1, the ion caustic wave enhancement activities are still often observed in the BLs, which makes it difficult to ex- plain them by the traditional plasma theory. New results reported in this paper further show that the magnetic cloud’s BL is an important dynamic structure, which could provide useful diagnosis for understanding the cloud’s BL physics and could expand a space developing space plasma wave theory.

Three-dim ensional MHD simulation for the solar wind structure observed by Ulysses

Ulysses has been the first spacecraft to explore the high latitudinal regions of the heliosphere till now. During its first rapid pole-to-pole transit from September 1994 to June 1995, Ulysses observed a fast speed flow with magnitude reaching 700—800 km/s at high latitudinal region except 20°area near the ecliptic plane where the velocity is 300—400 km/s. The observations also showed a sudden jump of the velocity across the two regions. In this note, based on the characteristic and representative observations of the solar magnetic field and K-coronal polarized brightness, the large-scale solar wind structure mentioned above is reproduced by using a three-dimensional MHD model. The numerical results are basically consistent with those of Ulysses observations. Our results also show that the distributions of magnetic field and plasma number density on the solar source surface play an important role in governing this structure. Furthermore, the three-dimensional MHD model used here has a robust ability to simulate this kind of large-scale wind structure.

Recent progress in MHD simulations of the solar-terrestrial connection

In recent years,considerable efforts on Magnetohydrodynamic(MHD)simulation have been made to better understand the solar-terrestrial connection,i.e.the propagation and evolution of solar wind and solar storm as well as their effects on terrestrial system.This paper briefly reviews these works based on the selected publications during 2013–2014 that cover the solar and solar wind model,solar windMoon interaction model,solar wind-magnetosphere coupling model,and magnetospheric model,etc.