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Solar Intranetwork Magnetic Elements: bipolar flux appearance View all abstracts by submitter

Guiping Zhou   Submitted: 2012-02-29 02:46

The current study aims to quantify characteristic features of bipolar flux appearance of solar intranetwork (IN) magnetic elements. To attack such a problem, we use the Narrow-band Filter Imager (NFI) magnetograms from the Solar Optical Telescope (SOT) on board Hinode; these data are from quiet and an enhanced network areas. Cluster emergence of mixed polarities and IN ephemeral regions (ERs) are the most conspicuous forms of bipolar flux appearance within the network. Each of the clusters is characterized by a few well-developed ERs that are partially or fully co-aligned in magnetic axis orientation. On average, the sampled IN ERs have total maximum unsigned flux of several 1017 Mx separation of 3 - 4 arcsec, and a lifetime of 10 - 15 minutes. The smallest IN ERs have a maximum unsigned flux of several 1016 Mx, separations less than 1 arcsec, and lifetimes as short as 5 minutes. Most IN ERs exhibit a rotation of their magnetic axis of more than 10 degrees during flux emergence. Peculiar flux appearance, e.g., bipole shrinkage followed by growth or the reverse, is not unusual. A few examples show repeated shrinkage-growth or growth-shrinkage, like magnetic floats in the dynamic photosphere. The observed bipolar behavior seems to carry rich information on magneto-convection in the sub-photospheric layer.

ADMIN: Authors have been asked to supply a preprint which should be available within a day or two

Authors: Jingxiu Wang; Guiping Zhou; Chunlan Jin; Hui Li
Projects: Very Large Array

Publication Status: in press
Last Modified: 2012-02-29 08:24
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