High Resolution Studies of Solar Flares, Active Regions, Prominences and the Quiet Sun at Centimeter and Millimeter Wavelengths

了解太阳活动和太阳耀斑仍然是 科技研究中最重要的未解决的问题。 近几 几十年来，数据收集的迅速发展，特别是从 卫星和无线电领域，都导致了更大的 理解和更好地理解 问题所在 太阳活动的基本原因是 从广义上理解。 太阳底下的对流区 光球层负责差异旋转和 磁场的产生，它的迅速出现，通过 曲面创建活动区域。 太阳耀斑代表了 日冕耀斑爆发前储存的能量突然释放 太阳的大气层。 能量可以作为自由能储存起来。 载流磁场的能量。 基本 所有耀斑模型或磁场配置的要求 能量的储存必须处于亚稳态：稳定 但对大扰动不稳定， 导致存储能量的脉冲释放。 不同的耀斑模型的特点是特定的 电晕中的磁场结构，以及爆炸物 磁场的重新连接。 理论磁场 配置可以进行观测测试，使用 强度和偏振图与VLA。 高 VLA和厘米提供的空间分辨率 VLA工作的波长非常适合于 确定所述张开区域的磁场结构。 特别是，使用不同波长的无线电波， 可以探索太阳大气层的不同层次。 无线电 观察也是独特的，因为它们提供了重要的 关于燃烧时磁场强度的信息 地区

Understanding solar activity and solar flares remains one of the most important unsolved problems in S/T research. In recent decades the rapid expansion in data gathering, particularly from satellites and in the radio domain, has led both to a greater understanding and to a better appreciation of the complexity of the problem. The basic causes of solar activity are now understood in broad terms. The convective zone beneath the solar photosphere is responsible for differential rotation and for the generation of magnetic fields, whose rapid emergence through the surface creates an active region. A solar flare represents the sudden release of energy stored before the flare in the coronal region of the sun's atmosphere. Energy may be stored as the free energy of a current-carrying magnetic field. The basic requirement of all flare models or magnetic field configurations is that storage of energy must be in a metastable state: stable to small perturbations but unstable to large perturbations, which lead to the impulsive release of stored energy. The different flare models are characterized by specific magnetic field configurations in the corona, and by the explosive reconnection of magnetic fields. The theoretical magnetic field configurations can be subjected to observational tests using intensity and polarization maps made with the VLA. The high spatial resolution available with the VLA and the centimeter wavelengths at which the VLA operates are ideally suited for determining the magnetic field structures of the flaring region. In particular, using radio waves of different wavelengths, one can explore different levels of the sun's atmosphere. Radio observations are also unique in that they provide important information on the strength of the magnetic field in flaring regions.