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Dynamics of Coronal Bright Points as seen by Sun Watcher using Active Pixel System detector and Image Processing (SWAP), Atmospheric Imaging Assembly AIA), and Helioseismic and Magnetic Imager (HMI) View all abstracts by submitter

Chandrahekhar Kalugodu   Submitted: 2012-06-05 04:48

The extit{Sun Watcher using Active Pixel system detector and Image Processing}(SWAP) on board the extit{PRoject for OnBoard Autonomy odash 2} (PROBA odash 2) spacecraft provides images of the solar corona in EUV channel centered at 174 AA. These data, together with extit{Atmospheric Imaging Assembly} (AIA) and the extit{Helioseismic and Magnetic Imager} (HMI) on board extit{Solar Dynamics Observatory} (SDO), are used to study the dynamics of coronal bright points. The evolution of the magnetic polarities and associated changes in morphology are studied using magnetograms and multi-wavelength imaging. The morphology of the bright points seen in low-resolution SWAP images and high-resolution AIA images show different structures, whereas the intensity variations with time show similar trends in both SWAP 174 and AIA 171 channels. We observe that bright points are seen in EUV channels corresponding to a magnetic-flux of the order of 1018 Mx. We find that there exists a good correlation between total emission from the bright point in several UV odash EUV channels and total unsigned photospheric magnetic flux above certain thresholds. The bright points also show periodic brightenings and we have attempted to find the oscillation periods in bright points and their connection to magnetic flux changes. The observed periods are generally long (10 odash 25 minutes) and there is an indication that the intensity oscillations may be generated by repeated magnetic reconnection.

Authors: K. Chandrashekhar, S. Krishna Prasad, D. Banerjee, B. Ravindra, Daniel B. Seaton
Projects: None

Publication Status: Accepted for publication in Solar Physics
Last Modified: 2012-06-05 10:40
Go to main E-Print page  Solar Coronal Loops Resolved by Hinode and SDO  Determination of the acceleration region size in a loop-structured solar flare   Edit Entry  Download Preprint  Delete Entry 

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