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Determination of the Coronal Magnetic Field by Hot Loop Oscillations Observed by SUMER and SXT View all abstracts by submitter

Tongjiang Wang   Submitted: 2006-10-30 21:29

We apply a new method to determine the magnetic field in coronal loops using observations of coronal loop oscillations. We analyze seven Doppler shift oscillation events detected by SUMER in the hot flare line Fe XIX to obtain oscillation periods of these events. The geometry, temperature, and electron density of the oscillating loops are measured from coordinated multi-channel soft X-ray imaging observations from SXT. All the oscillations are consistent with standing slow waves in their fundamental mode. The parameters are used to calculate the magnetic field of coronal loops based on MHD wave theory. For the seven events, the plasma eta is in the range 0.15-0.91 with a mean of 0.33pm0.26, and the estimated magnetic field varies between 21-61 G with a mean of 34pm14 G. With background emission subtracted, the estimated magnetic field is reduced by 9%-35%. The maximum backgroud subtraction gives a mean of 22pm13 G in the range 12-51 G. We discuss measurement uncertainties and the prospect of determining coronal loop magnetic fields from future observations of coronal loops and Doppler shift oscillations.

Authors: Tongjiang Wang, Davina E. Innes, and Jiong Qiu
Projects: SoHO-SUMER

Publication Status: ApJ, V656, No. 1, Feb 10 2007 issue
Last Modified: 2006-10-31 12:06
Go to main E-Print page  THE EVAPORATION REGIME IN A CONFINED FLARE  Analysis of power spectra of Doppler shift time series as a diagnostic tool for coronal loops  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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