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Statistical Study on the Nature of Solar Flux Emergence View all abstracts by submitter

Kenichi Otsuji   Submitted: 2011-06-12 20:09

We studied 101 flux emergence events ranging from small ephemeral regions tolarge emerging flux regions which were observed with Hinode Solar OpticalTelescope filtergram. We investigated how the total magnetic flux of theemergence event controls the nature of emergence. To determine the modes ofemergences, horizontal velocity fields of global motion of the magnetic patchesin the flux emerging sites were measured by the local correlation tracking.Between two main polarities of the large emerging flux regions with more thanaround 2 imes 1019 Mx, there were the converging flows of anti-polaritymagnetic patches. On the other hand, small ephemeral regions showed noconverging flow but simple diverging pattern. When we looked into the detailedfeatures in the emerging sites, irrespective of the total flux and the spatialsize, all the emergence events were observed to consist of single or multipleelementary emergence unit(s). The typical size of unitary emergence is 4 Mm andconsistent with the simulation results. From the statistical study of the fluxemergence events, the maximum spatial distance between two main polarities, themagnetic flux growth rate and the mean separation speed were found to followthe power-law functions of the total magnetic flux with the indices of 0.27,0.57, and -0.16, respectively. From the discussion on the observed power-lawrelations, we got a physical view of solar flux emergence that emergingmagnetic fields float and evolve balancing to the surrounding turbulentatmosphere. Key words: Sun: magnetic fields - Sun: emerging flux - Sun:photosphere - Sun: chromosphere

Authors: Kenichi Otsuji, Reizaburo Kitai, Kiyoshi Ichimoto, Kazunari Shibata
Projects: Hinode/SOT,SoHO-MDI

Publication Status: Accepted
Last Modified: 2011-06-14 19:51
Go to main E-Print page  The 2011/02/15 X2 flare, ribbons, coronal wave, and mass ejection: interpreting the 3-d views from SDO and STEREO guided by MHD flux-rope modeling  Patchy Reconnection in the Solar Corona  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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