日冕物质抛射的三维数值模拟研究
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摘要
空间天气研究涵盖太阳日冕、行星际、磁层、电离层、中高层大气等物理性质不同的空间区域,空间灾害性事件的日冕-行星际过程是空间天气研究的主要内容之一,而基于磁流体力学(MHD)方程组的数值模型是研究该内容的有力工具,可以为近地空间天气变化研究提供科学输入。本文首先发展了日冕-行星际CESE模式(SIP-CESE Model),然后应用该模式模拟研究了1997年5月12日CME事件和1998年11月4-5日的三个续发CMEs事件在日冕-行星际空间的三维传播与演化过程,其中的三维背景太阳风采用磁场的观测数据做为初始输入通过时间松弛法求解3D时变MHD方程得到,行星际扰动参数尽量由观测数据决定。
针对太阳风的球形计算区域,把整个空间剖分成非重叠的五面体网格结构,在此网格基础上,建立了基于CESE格式的日冕-行星际耦合的MHD模式(SIP-CESE MHD Model),该模式可以模拟从1Rs到近地轨道(215Rs)附近的三维背景太阳风。作为该格式的验证,分别采用多极磁场和观测的太阳表面磁场输入通过时间松弛法求解3D MHD方程组模拟了两个日冕定态解。证明该模式具有以下优点:它将时间和空间统一起来同等对待;在给出网格点物理量值的同时也给出了物理量的偏导数;可以满意地求解间断流场,具有较高的分辨率;构造比较简单,除了简单的Taylor展开之外,没有采用其他的数值方法。
接着,用新发展的日冕-行星际CESE MHD模式模拟日地联系事件-1997年5月12日CME事件。和该事件的其它数值模拟相比,本文数值格式的主要特征是:(1)通过输入观测的光球磁场,由3D时变数值MHD模型得到背景太阳风;(2)瞬变扰动是从太阳表面触发,添加扰动的位置、角宽度和实际观测数据一致。模拟结果和WIND飞船观测数据比较相对比较满意。证明此数值模式可以基本模拟三维真实CME在日冕-行星际空间的传播和演化过程。
Burlaga et al. (2002)指出大约仅有三分之一的对地方向的太阳物质抛射在地球附近形成磁云(MC);大部分喷发形成复杂抛射或者多重MCs(在地球附近,仍然可以区分不同的MCs)。同一活动区的多个续发CMEs提供了研究对地过程中多个CMEs相互作用的很好的例子。用新发展的日冕-行星际CESEMHD模式模拟了1998年11月4日至5日起源于8375活动区的3个连续日冕物质抛射在行星际空间的传播和相互作用并最终形成复杂抛射体的日地传输过程。三维背景太阳风用Parker一维太阳风解和太阳光球磁场观测数据作为输入得到。该模拟中,三次事件的触发位置和实际观测位置一致,CME的扰动参数,如速度、方向和角宽度由SOHO/LASCO的观测数据并结合锥模型来确定。模拟结果可以重现和解释飞船观测的复杂抛射的一些一般特征。
The space weather research includes a number of di?erent physics domains:solar corona, inner heliosphere, magnetosphere, ionosphere electrodynamics, andupper atmosphere and so on. The solar-interplanetary propagation process of thespace disaster weather is one of the most important contents of the space weatherresearch. The magnetohydrodynamic(MHD) modeling plays an very importantrole in studying the process, and can provide appropriate conditions for coupledmodel of magnetosphere, ionosphere electrodynamics, and upper atmosphere.In this paper, we develop solar-interplanetary CESE MHD model(SIP-CESEmodel). Then, we use our newly developed SIP-CESE MHD model to simu-late three-dimensional characters of the propagation and transit process of 12May 1997 CME event and three successive Coronal Mass Ejections (CMEs) ofNovember 4-5, 1998 from sun to earth. In these studies, the three-dimensionalbackground solar wind is derived from a 3D time-dependent numerical MHDmodel by input measured photospheric magnetic fields. The initiation of theseCMEs is partially determined from spacecraft observations.
In order to establish 3D model in the spherical shell, a grid system of non-overlapped pentahedron is constructed. Based on the 3-D grid structure, weintegrate numerical models of the Solar Corona, Inner Heliosphere into a coupledmodel (SIP-CESE MHD Model). The model can simulate the three-dimensionalbackground solar wind from Sun to Earth. As validation of the SIP-CESE MHDModel, the model is applied to 3-dimensional MHD equations by time-relaxationapproach, with the purpose of modeling the steady-state solar atmospheric studyby using multipole magnetic fields and measured solar surface magnetic fields,respectively. The model has many advantages. Firstly, space and time are uni-fied and treated on the same footing. Secondly, the gradients of ?ow variablesare solved simultaneously as independent unknowns. Thirdly, It is capable ofhandling both continuous and discontinuous ?ows very well. Finally, no ap-proximation techniques other than Taylor’s series expansion are employed in this method, so the computational logic of the present method is considerably simpler.
Afterwards, Our newly developed SIP-CESE MHD model is used to simu-late sun-earth connection event with the well-studied 12 May 1997 CME event asan example. The main features and approximations of our numerical model are(1) the background solar wind is derived from a 3D time-dependent numericalMHD model by input measured photospheric magnetic fields and (2) transientdisturbances are derived from solar surface by introducing a mass ?ow of hotplasma. In our simulation, the initial parameters of the CME, such as directionand angular size of the expanding CME, are determined from the observationdata. The numerical simulation provided us with a relatively satisfactory com-parison with the WIND spacecraft observations. This shows that this numericalmodel has capability in modeling realistic 3-dimensional CME.
According to Burlaga et al. (2002), only about one-third of Earth directedsolar eruptions leads to the passage of an MC at Earth; the majority of the ejec-tions form either complex ejecta or multiple MCs (when the di?erent MCs in theejecta can still be distinguished at Earth). Homologous eruptions provide a goodexample of potential interactions of CMEs on their way to Earth. We present thesolar-terrestrial transit process of three successive CMEs of November 4-5, 1998originating from active region 8375 by using newly developed SIP-CESE MHDmodel. These CMEs interact with each other while they are propagating in inter-planetary space and finally form a complex ejecta. The quiet solar wind is startedfrom Parker-like 1D solar wind solution and the magnetic field map calculatedfrom the solar photospheric magnetic field data. In our simulation, the ejectionsare initiated using pulse in the real active region 8375. The initial parametersof the CMEs , such as speed, direction and angular size of the expanding CME,are determined from the SOHO/LASCO data with the Cone-model. The resultsshow that our simulation can reproduce and explain some of the general featuresobserved by satellite for the complex ejecta.
针对太阳风的球形计算区域,把整个空间剖分成非重叠的五面体网格结构,在此网格基础上,建立了基于CESE格式的日冕-行星际耦合的MHD模式(SIP-CESE MHD Model),该模式可以模拟从1Rs到近地轨道(215Rs)附近的三维背景太阳风。作为该格式的验证,分别采用多极磁场和观测的太阳表面磁场输入通过时间松弛法求解3D MHD方程组模拟了两个日冕定态解。证明该模式具有以下优点:它将时间和空间统一起来同等对待;在给出网格点物理量值的同时也给出了物理量的偏导数;可以满意地求解间断流场,具有较高的分辨率;构造比较简单,除了简单的Taylor展开之外,没有采用其他的数值方法。
接着,用新发展的日冕-行星际CESE MHD模式模拟日地联系事件-1997年5月12日CME事件。和该事件的其它数值模拟相比,本文数值格式的主要特征是:(1)通过输入观测的光球磁场,由3D时变数值MHD模型得到背景太阳风;(2)瞬变扰动是从太阳表面触发,添加扰动的位置、角宽度和实际观测数据一致。模拟结果和WIND飞船观测数据比较相对比较满意。证明此数值模式可以基本模拟三维真实CME在日冕-行星际空间的传播和演化过程。
Burlaga et al. (2002)指出大约仅有三分之一的对地方向的太阳物质抛射在地球附近形成磁云(MC);大部分喷发形成复杂抛射或者多重MCs(在地球附近,仍然可以区分不同的MCs)。同一活动区的多个续发CMEs提供了研究对地过程中多个CMEs相互作用的很好的例子。用新发展的日冕-行星际CESEMHD模式模拟了1998年11月4日至5日起源于8375活动区的3个连续日冕物质抛射在行星际空间的传播和相互作用并最终形成复杂抛射体的日地传输过程。三维背景太阳风用Parker一维太阳风解和太阳光球磁场观测数据作为输入得到。该模拟中,三次事件的触发位置和实际观测位置一致,CME的扰动参数,如速度、方向和角宽度由SOHO/LASCO的观测数据并结合锥模型来确定。模拟结果可以重现和解释飞船观测的复杂抛射的一些一般特征。
The space weather research includes a number of di?erent physics domains:solar corona, inner heliosphere, magnetosphere, ionosphere electrodynamics, andupper atmosphere and so on. The solar-interplanetary propagation process of thespace disaster weather is one of the most important contents of the space weatherresearch. The magnetohydrodynamic(MHD) modeling plays an very importantrole in studying the process, and can provide appropriate conditions for coupledmodel of magnetosphere, ionosphere electrodynamics, and upper atmosphere.In this paper, we develop solar-interplanetary CESE MHD model(SIP-CESEmodel). Then, we use our newly developed SIP-CESE MHD model to simu-late three-dimensional characters of the propagation and transit process of 12May 1997 CME event and three successive Coronal Mass Ejections (CMEs) ofNovember 4-5, 1998 from sun to earth. In these studies, the three-dimensionalbackground solar wind is derived from a 3D time-dependent numerical MHDmodel by input measured photospheric magnetic fields. The initiation of theseCMEs is partially determined from spacecraft observations.
In order to establish 3D model in the spherical shell, a grid system of non-overlapped pentahedron is constructed. Based on the 3-D grid structure, weintegrate numerical models of the Solar Corona, Inner Heliosphere into a coupledmodel (SIP-CESE MHD Model). The model can simulate the three-dimensionalbackground solar wind from Sun to Earth. As validation of the SIP-CESE MHDModel, the model is applied to 3-dimensional MHD equations by time-relaxationapproach, with the purpose of modeling the steady-state solar atmospheric studyby using multipole magnetic fields and measured solar surface magnetic fields,respectively. The model has many advantages. Firstly, space and time are uni-fied and treated on the same footing. Secondly, the gradients of ?ow variablesare solved simultaneously as independent unknowns. Thirdly, It is capable ofhandling both continuous and discontinuous ?ows very well. Finally, no ap-proximation techniques other than Taylor’s series expansion are employed in this method, so the computational logic of the present method is considerably simpler.
Afterwards, Our newly developed SIP-CESE MHD model is used to simu-late sun-earth connection event with the well-studied 12 May 1997 CME event asan example. The main features and approximations of our numerical model are(1) the background solar wind is derived from a 3D time-dependent numericalMHD model by input measured photospheric magnetic fields and (2) transientdisturbances are derived from solar surface by introducing a mass ?ow of hotplasma. In our simulation, the initial parameters of the CME, such as directionand angular size of the expanding CME, are determined from the observationdata. The numerical simulation provided us with a relatively satisfactory com-parison with the WIND spacecraft observations. This shows that this numericalmodel has capability in modeling realistic 3-dimensional CME.
According to Burlaga et al. (2002), only about one-third of Earth directedsolar eruptions leads to the passage of an MC at Earth; the majority of the ejec-tions form either complex ejecta or multiple MCs (when the di?erent MCs in theejecta can still be distinguished at Earth). Homologous eruptions provide a goodexample of potential interactions of CMEs on their way to Earth. We present thesolar-terrestrial transit process of three successive CMEs of November 4-5, 1998originating from active region 8375 by using newly developed SIP-CESE MHDmodel. These CMEs interact with each other while they are propagating in inter-planetary space and finally form a complex ejecta. The quiet solar wind is startedfrom Parker-like 1D solar wind solution and the magnetic field map calculatedfrom the solar photospheric magnetic field data. In our simulation, the ejectionsare initiated using pulse in the real active region 8375. The initial parametersof the CMEs , such as speed, direction and angular size of the expanding CME,are determined from the SOHO/LASCO data with the Cone-model. The resultsshow that our simulation can reproduce and explain some of the general featuresobserved by satellite for the complex ejecta.
引文
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