Are Moreton waves coronal phenomena?

被引：27

作者：

Balasubramaniam, K. S. ^{[1
]}

Pevtsov, A. A. ^{[1
]}

Neidig, D. F. ^{[1
]}

机构：

[1] Natl Solar Observ, Sunspot, NM 88349 USA

来源：

ASTROPHYSICAL JOURNAL | 2007年 / 658卷 / 02期

关键词：

stars : activity; stars : coronae; stars : chromospheres; stars : magnetic fields; Sun : activity; Sun : chromosphere; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : flares; Sun : magnetic fields; waves;

D O I：

10.1086/512001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on permeability characteristics of the upper solar atmosphere due to the progression of a Moreton wave. An exceptional Moreton wave is tracked to cover most of the Sun, following an unusually large solar X- ray flare observed on 2003 October 29. Using H alpha intensity and Doppler measurements, the Moreton wave is tracked for as long as 12 minutes. Moving outward, the wave circumnavigates strong-field active regions. The wave sweeps through solar magnetic neutral lines, disrupting material from filament and filament channels, thereby accentuating the visibility of the wave. We establish that the requirement for the visibility of a Moreton wave is the necessary presence of higher density material in the layers of the corona, besides reaffirming that Moreton waves are observed only when the speed of the disturbance exceeds Mach 2. We suggest that the cause can be a removal of significant amount of material from the solar upper atmosphere due to a coronal mass ejection.

引用

页码：1372 / 1379

页数：8

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