Calculating the Thermal Structure of Solar Active Regions in Three Dimensions
Calculating the Thermal Structure of Solar Active Regions in Three Dimensions
复制标题
DOI：
10.1086/427739
复制
发表时间：
2005-03
期刊：
影响因子：
--
通讯作者：
Y. Mok;Z. Mikić;R. Lionello;J. Linker
中科院分区：
文献类型：
--
作者：
Y. Mok;Z. Mikić;R. Lionello;J. Linker
我们描述了一种技术，以获得一个特定的等离子体加热模型的温度和密度分布在一个活跃的区域。该技术可普遍应用于自洽确定磁场和热结构。为了简单起见，我们说明了这种技术的应用在小等离子体β的限制，其中等离子体动力学从磁场的，一个很好的近似在活动区域，其中磁场是强的。我们选择了一个特定的活动区域，观察在1996年8月，以证明的方法。我们将该技术应用于一个无力的磁场与等离子体加热模型，其中体积日冕加热速率与局部磁场的强度成正比，我们计算预期的极紫外线和软X射线发射从所产生的热结构。我们比较我们的解决方案与一维回路模型和分析回路标度律。在未来，我们计划将这些发射图像与SOHO EUV成像望远镜（EIT）和Yohkoh软X射线望远镜（SXT）获得的图像进行比较，并探索日冕发射和各种日冕加热模型之间的关系。
We describe a technique to obtain the temperature and density distribution in an active region for a specified plasma heating model. The technique can be applied in general to determine the magnetic field and thermal structure self-consistently. For simplicity, we illustrate the application of this technique in the limit of small plasma β, in which the plasma dynamics decouples from that of the magnetic field, a good approximation in active regions, in which the magnetic field is strong. We select a particular active region, observed in 1996 August, to demonstrate the methodology. We apply the technique to a force-free magnetic field with a plasma heating model in which the volumetric coronal heating rate is directly proportional to the strength of the local magnetic field, and we compute the expected extreme-ultraviolet and soft X-ray emissions from the resulting thermal structure. We compare our solutions with one-dimensional loop models and analytic loop scaling laws. In the future, we plan to compare these emission images with those obtained by the SOHO EUV Imaging Telescope (EIT) and the Yohkoh Soft X-Ray Telescope (SXT) and to explore the relationship between coronal emission and various coronal heating models.