Excitation of transverse magnetic tube waves in stellar convection zones. II. Wave energy spectra and fluxes
Excitation of transverse magnetic tube waves in stellar convection zones. II. Wave energy spectra and fluxes
复制标题
恒星对流区横向磁管波的激发。
DOI：
10.1051/0004-6361:20011834
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发表时间：
2002
影响因子：
6.5
通讯作者：
P. Ulmschneider
中科院分区：
文献类型：
--
作者：
Z. Musielak;P. Ulmschneider
利用本系列前一篇论文中所发展的解析方法，计算了恒星对流区中产生的横向磁管波的波能谱和通量。产生这些波的主要物理过程是外部湍流对流对细且垂直取向的磁通量管的摇动。该方法包含了当磁管在其相当大一部分长度上被摇动时出现的关联效应，但仅限于线性波。计算是针对有效温度从\(T_{eff}=2000K\)到\(10000K\)，重力加速度\(\log g = 3 - 5\)的星族I恒星进行的。结果表明，线性横向波沿单个磁通量管携带的通量比线性纵向磁管波携带的通量大约高一个数量级。所得结果可用于构建恒星色球层和星风的理论模型。
The wave energy spectra and fluxes for transverse magnetic tube waves generated in stellar convection zones are computed by using the analytical method developed in the previous paper of this series. The main physical process responsible for the generation of these waves is shaking of a thin and vertically oriented magnetic flux tube by the external turbulent convection. The approach includes the correlation effects, which occur when the tube is shaken over a significant fraction of its length, but is limited to linear waves. The calculations are performed for population I stars with effective temperatures ranging from T e f f = 2000 K to 10000 K, and with gravities log g = 3-5. It is shown that the fluxes carried by linear transverse waves along a single flux tube are approximately one order of magnitude higher than those carried by linear longitudinal tube waves. The obtained results can be used to construct theoretical models of stellar chromospheres and winds.