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Detection of ultra-long-period oscillations in an EUV filament View all abstracts by submitter

Claire Foullon   Submitted: 2004-09-29 04:26

We report the first detection of long-period (8-27 hours) oscillatory intensity variations in a coronal filament. The filament is observed continuously as it crosses the solar disk in a 12-minute-cadence SoHO/EIT 195 A, uninterrupted data set. Cyclic intensity variations are found to be correlated along the filament, while the most pronounced oscillations are detected at its southern end for nearly 6 days. The dominant period of these oscillations is 12.1 hours and the amplitude of the intensity variations reaches approximately 10% of the background intensity. The ultra-long-period oscillations may be interpreted in terms of slow string MHD modes or may be connected with thermal over-stability associated with peculiarities of the cooling/heating function and with the effect of neutrals. These theoretical predictions however do not explain the spatial structure of the oscillations along the filament.

Authors: Foullon C., Verwichte E. and Nakariakov V.M.
Projects: Soho-EIT

Publication Status: A&A 427, L5-L8
Last Modified: 2004-10-26 02:47
Go to main E-Print page  The role of observed MHD oscillations and waves for coronal heating (Invited Review)  Reconstruction of a Magnetohydrodynamic Velocity Field Vector 
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