NONLINEAR DAMPING OF ALFVEN WAVES IN THE SOLAR CORONA BELOW 1.5 SOLAR RADII

被引：8

作者：

Zhao, J. S. ^{[1
,2
]}

Voitenko, Y. ^{[3
]}

Guo, Y. ^{[4
,5
]}

Su, J. T. ^{[2
]}

Wu, D. J. ^{[1
]}

机构：

[1] Chinese Acad Sci, Key Lab Planetary Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China

[2] Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China

[3] Belgian Inst Space Aeron, Space Phys Div, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium

[4] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210046, Jiangsu, Peoples R China

[5] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210046, Jiangsu, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 811卷 / 02期

关键词：

magnetohydrodynamics (MHD); solar wind; Sun: corona; waves; MAGNETOHYDRODYNAMIC TURBULENCE; WIND ACCELERATION; LINE WIDTHS; ENERGY; HOLES; PROPAGATION; PHOTOSPHERE; SIMULATION; GENERATION; FIELDS;

D O I：

10.1088/0004-637X/811/2/88

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Nonthermal velocities measured in the solar corona imply a strong damping of upward-propagating low-frequency less than or similar to 0.01 Hz Alfven waves at heliocentric distances from 1.02 to 1.4 solar radii. We propose a vector Alfven wave decay as a feasible mechanism for the observed Alfven wave damping. Contrary to the extensively studied scalar decay, the vector decay does not depend on the wave frequency and can be efficient for low-frequency coronal Alfven waves. We show that the vector decay is much stronger than the scalar decay and can provide the observed damping of 0.01 Hz coronal Alfven waves with perpendicular wavelengths of similar to 10(4) km or less. Fully three-dimensional (3D) numerical simulations are needed to capture this decay, whose growth rate is proportional to the vector product of interacting wave vectors.

引用

页数：6

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