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Title:
Are Moreton Waves Coronal Phenomena?
Authors:
Balasubramaniam, K. S.; Pevtsov, A. A.; Neidig, D. F.
Affiliation:
AA(National Solar Observatory, Sunspot, NM 88349; , , ), AB(National Solar Observatory, Sunspot, NM 88349; , , ), AC(National Solar Observatory, Sunspot, NM 88349; , , )
Publication:
The Astrophysical Journal, Volume 658, Issue 2, pp. 1372-1379. (ApJ Homepage)
Publication Date:
04/2007
Origin:
UCP
ApJ Keywords:
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
DOI:
10.1086/512001
Bibliographic Code:
2007ApJ...658.1372B

Abstract

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 Hα 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.
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