MHD turbulence and heating of the open field-line solar corona

被引：21

作者：

Matthaeus, WH ^{[1
]}

Mullan, DJ

Dmitruk, P

Milano, L

Oughton, S

机构：

[1] Univ Delaware, Newark, DE 19716 USA

[2] Univ Waikato, Hamilton, New Zealand

来源：

NONLINEAR PROCESSES IN GEOPHYSICS | 2003年 / 10卷 / 1-2期

基金：

美国国家科学基金会;

关键词：

D O I：

10.5194/npg-10-93-2003

中图分类号：

P [天文学、地球科学];

学科分类号：

07 ;

摘要：

This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations. Reflection from coronal inhomogeneities plays an important role in sustaining the cascade. Physical and observational constraints are discussed. Kinetic processes that convert cascaded energy into heat must occur in regions of turbulent small-scale reconnection, and may be similar in some respects to ion heating due to intense electron beams observed in the aurora.

引用

页码：93 / 100

页数：8

共 48 条

[1] REFLECTION AND TRAPPING OF ALFVEN WAVES IN A SPHERICALLY SYMMETRIC STELLAR ATMOSPHERE [J].