Evolution of coronal magnetic fields

日冕磁场的演化

• 批准号: 168925481
• 负责人: Dr. Thomas Wiegelmann
• 金额: --
• 依托单位: Max-Planck-Institut für Sonnensystemforschung (MPS)
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2010
• 资助国家: 德国
• 起止时间: 2009-12-31 至 2012-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/168925481?language=en
• 关键词: Evolution; coronal; magnetic; fields

Solar eruptions like flares and coronal mass ejections expel a huge amount of energy in the form of radiation and charged particles into the interplanetary space. These cause impressive phenomena at Earth like aurorae but also have harmful effects like the disruption of radio communication, the damage of satellites, and power cutoffs. These eruptions are driven by instabilities of the coronal magnetic field. High-accuracy routine measurements of the magnetic field vector are restricted to the photosphere and one needs to apply extrapolation techniques to reconstruct the coronal magnetic field. Within this work we plan to apply the sophisticated nonlinear force-free approach to compute the three-dimensional coronal magnetic field structure from a series of photospheric vector magnetograms with unprecedented high spacial and temporal resolution. Our aims are on one hand to study the temporal evolution of the magnetic energy, helicity, topology and current sheet formation in the solar corona to understand and predict eruptive phenomena. On the other hand we aim to study the coronal plasma guided by the reconstructed magnetic field lines in order to get insights into physical processes of the coronal plasma, in particular coronal heating.

耀斑和日冕物质抛射等太阳喷发以辐射和带电粒子的形式将大量能量释放到行星际空间中。它们会在地球上造成极光等令人印象深刻的现象，但也会产生有害影响，例如无线电通信中断、卫星损坏和断电。这些喷发是由日冕磁场的不稳定驱动的。磁场矢量的高精度常规测量仅限于光球层，需要应用外推技术来重建日冕磁场。在这项工作中，我们计划应用复杂的非线性无力方法，从一系列具有前所未有的高空间和时间分辨率的光球矢量磁图计算三维日冕磁场结构。我们的目标一方面是研究日冕中磁能、螺旋度、拓扑结构和电流片形成的时间演化，以了解和预测喷发现象。另一方面，我们的目标是研究由重建的磁场线引导的日冕等离子体，以便深入了解日冕等离子体的物理过程，特别是日冕加热。

项目成果

How Should One Optimize Nonlinear Force-Free Coronal Magnetic Field Extrapolations from SDO/HMI Vector Magnetograms?

• DOI: 10.1007/s11207-012-9966-z
• 发表时间: 2012-02
• 期刊: Solar Physics
• 影响因子: 2.8
• 作者: T. Wiegelmann;J. Thalmann;B. Inhester;T. Tadesse;Xudong Sun;J. Hoeksema

COMPARISON OF FORCE-FREE CORONAL MAGNETIC FIELD MODELING USING VECTOR FIELDS FROM HINODE AND SOLAR DYNAMICS OBSERVATORY

• DOI: 10.1088/0004-637x/769/1/59
• 发表时间: 2013-04
• 期刊: The Astrophysical Journal
• 作者: J. Thalmann;S. Tiwari;T. Wiegelmann

EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION

基于 SDO/HMI 观测的主要喷发活跃区磁场和能量的演化

• DOI: 10.1088/0004-637x/748/2/77
• 发表时间: 2012
• 期刊: The Astrophysical Journal
• 作者: Hoeksema;Wiegelmann;T.Hayashi;Thalmann
• 通讯作者: Thalmann

FORCE-FREE FIELD MODELING OF TWIST AND BRAIDING-INDUCED MAGNETIC ENERGY IN AN ACTIVE-REGION CORONA

活动区电晕中扭曲和编织感应磁场的无力场建模

• DOI: 10.1088/0004-637x/780/1/102
• 发表时间: 2014
• 期刊: The Astrophysical Journal
• 作者: Thalmann;Tiwari;Wiegelmann
• 通讯作者: Wiegelmann

NONLINEAR FORCE-FREE FIELD MODELING OF A SOLAR ACTIVE REGION USING SDO/HMI AND SOLIS/VSM DATA

使用 SDO/HMI 和 SOLIS/VSM 数据对太阳能活动区域进行非线性无力场建模

• DOI: 10.1088/0004-6256/144/2/33
• 发表时间: 2012
• 期刊: The Astronomical Journal
• 作者: Thalmann;Pietarila;Wiegelmann
• 通讯作者: Wiegelmann