We have undertaken a major enhancement of our IDL-based simulation tools developed earlier for modeling microwave and X-ray emission. The object-based architecture provides an interactive graphical user interface that allows the user to import photospheric magnetic field maps and perform magnetic field extrapolations to almost instantly generate 3D magnetic field models, to investigate the magnetic topology of these models by interactively creating magnetic field lines and associated magnetic flux tubes, to populate the flux tubes with user-defined nonuniform thermal plasma and anisotropic, nonuniform, nonthermal electron distributions; to investigate the spatial and spectral properties of radio and X-ray emission calculated from the model, and to compare the model-derived images and spectra with observational data. The application integrates shared-object libraries containing fast gyrosynchrotron emission codes developed in FORTRAN and C++, soft and hard X-ray codes developed in IDL, a FORTRAN-based potential-field extrapolation routine and an IDL-based linear force free field extrapolation routine. The interactive interface allows users to add any user-defined radiation code that adheres to our interface standards, as well as user-defined magnetic field extrapolation routines. Here we use this tool to analyze a simple single-loop flare and use the model to constrain the 3D structure of the magnetic flaring loop and 3D spatial distribution of the fast electrons inside this loop. We iteratively compute multi-frequency microwave and multi-energy X-ray images from realistic magnetic fluxtubes obtained from an extrapolation of a magnetogram taken prior to the flare, and compare them with imaging data obtained by SDO, NoRH, and RHESSI instruments. We use this event to illustrate use of the tool for general interpretation of solar flares to address disparate problems in solar physics.
Revealing Flare Energetics and Dynamics with SDO EVE Solar Extreme Ultraviolet Spectral Irradiance Observations
Laboratory for Atmospheric and Space Physics, University of Colorado（科罗拉多大学大气与空间物理实验室）；Johns Hopkins University, Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；High Altitude Observatory, National Center for Atmospheric Research（美国国家大气研究中心高空观测站）；Naval Research Laboratory（海军研究实验室）
Flare Energy Release at the Magnetic Field Polarity Inversion Line During M1.2 Solar Flare of 2015 March 15. II. Investigation of Photospheric Electric Current and Magnetic Field Variations Using HMI 135-second Vector Magnetograms
Multiwavelength Observations of the Precursors Before the Eruptive X4.9 Limb Solar Flare on 25 February, 2014: Current Sheet, Eruptive Filament, Flare and Eruption Onset in the Frame of the Tether-Cutting Magnetic Reconnection Scenario
Three-dimensional mapping of coronal magnetic field and plasma parameters in a solar flare
Institut für Sonnenphysik (KIS)（太阳物理研究所）；Center For Solar-Terrestrial Research, New Jersey Institute of Technology（新泽西理工学院太阳-地球关系研究中心）；University College London, Mullard Space Science Laboratory（伦敦大学学院穆拉德太空科学实验室）
Flare Energy Release in the Magnetic Field Polarity Inversion Line During M1.2 Solar Flare of March 15, 2015. Paper I. Onset of Plasma Heating and Electrons Acceleration
The Vertical Current Approximation Nonlinear Force-Free Field Code - Description, Performance Tests, and Measurements of Magnetic Energies Dissipated in Solar Flares
First Detailed MeerKAT Imaging Spectroscopy of a Solar Flare
University of Glasgow（格拉斯哥大学）；North-West University（西北大学）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；Northumbria University（诺森比亚大学）；Polish Academy of Sciences（波兰科学院）；New Jersey Institute of Technology（新泽西理工学院）；South African Radio Astronomy Observatory（南非射电天文台）；University of South Africa（南非大学）；UNISA Centre for Astrophysics and Space Sciences (UCASS)（UNISA天体物理学与空间科学中心）
Deep XMM-Newton observation of the Eta Chamaleontis cluster
Eta Chamaleontis星系团的成员正处于一个磁盘迅速演变的进化阶段。它还呈现出一些特点，如大部分的双星和吸积盘，可能与团簇形成过程有关。它的接近使这个恒星群成为研究X射线发射与这些恒星参数之间关系的理想目标。这项工作的主要目的是确定一般的X射线性质的集群成员的日冕温度，柱密度，发射措施，X射线光度和可变性。我们的目标也是建立这些恒星的X射线光度和其他恒星参数之间的关系，如双星和吸积盘的存在。本文还研究了每一次耀斑事件的耀斑能量及其与某些恒星参数的关系。我们使用的专有数据来自XMM-牛顿深度观测，指向Eta Chamaleontis星系团的核心。我们的观测使用了专门的XMM-牛顿数据简化软件进行分析。对于源的检测，我们使用基于小波的代码PWDetect。一般的日冕性质来自等离子体模型拟合。我们还确定了Eta Chamaleontis成员在EPIC视野中的变化。在五颗不同的恒星中，总共清楚地检测到六次类似耀斑的事件。分别推导了耀斑和伪静止状态下的日冕性质。在我们的观测中，经历过耀斑事件的恒星在伪静态下的X射线光度比具有相似光谱类型的没有耀斑迹象的星团成员高，无论它们是否具有吸积盘。观测到的耀斑能量是典型的主序前和主序星M。我们没有发现有和没有吸积盘的恒星的耀斑能量之间的差异。
