Emergence of magnetic flux from the convection zone into the solar atmosphere. I: Linear and nonlinear adiabatic evolution of the convective-Parker instability
Emergence of magnetic flux from the convection zone into the solar atmosphere. I: Linear and nonlinear adiabatic evolution of the convective-Parker instability
复制标题
磁通量从对流区进入太阳大气。
DOI：
--
复制
发表时间：
1992
期刊：
影响因子：
--
通讯作者：
R. Rosner
中科院分区：
文献类型：
--
作者：
S. Nozawa;K. Shibata;R. Matsumoto;A. Sterling;T. Tajima;Y. Uchida;A. Ferrari;R. Rosner
本文研究了太阳对流层出射的磁通量向光球层、色球层和日冕演化的线性和非线性性质。一个孤立的通量片（约400公里厚），最初嵌入一个简单的模型对流区（约1000-2000公里厚）下面的一个模型太阳大气是容易受到对流不稳定性和帕克不稳定性（磁浮力不稳定性的起伏模式）。对部分磁化对流区进行了线性稳定性分析，并利用二维MHD程序研究了系统的非线性演化
The linear and nonlinear properties of the evolution of emerging magnetic flux from the solar convection zone into the photosphere, chromosphere, and corona are studied. An isolated flux sheet (∼400 km thick) initially embedded in a simple model convection zone (∼1000-2000 km thick) below a model solar atmosphere is susceptible to both convective instability and the Parker instability (the undular mode of the magnetic buoyancy instability). A linear stability analysis of the partially magnetized convection zone is performed, and the nonlinear evolution of the system is studied with a two-dimensional MHD code