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Solar Physics

, Volume 278, Issue 2, pp 299–322 | Cite as

Solar Intranetwork Magnetic Elements: Bipolar Flux Appearance

  • Jingxiu Wang
  • Guiping Zhou
  • Chunlan Jin
  • Hui Li
Article
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Accepted:

Abstract

This study aims to quantify characteristic features of the bipolar flux appearance of solar intranetwork (IN) magnetic elements. To attack this problem, we use the Narrowband Filter Imager (NFI) magnetograms from the Solar Optical Telescope (SOT) on board Hinode; these data are from quiet and 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 coaligned in magnetic axis orientation. On average, the sampled IN ERs have a total maximum unsigned flux of several 1017 Mx, a 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 of 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 magnetoconvection in the subphotospheric layer.

Keywords

Sun: activity Sun: magnetic field Sun: photosphere Sun: intranetwork 
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Notes

Acknowledgements

The authors are grateful to the Hinode team for providing the data. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). Hinode SOT/SP inversions were done at the National Center for Atmospheric Research (NCAR) under the framework of the Community Spectro-polarimetric Analysis Center (CSAC; http://www.csac.hao.ucar.edu/ ). This work is supported by the National Natural Science Foundations of China (11003024, 10973019, 40974112, 11025315, 11003026, 10873038, 10833007 and 10921303), and the National Basic Research Program of China (G2011CB811403 and G2011CB811402), and the CAS Project KJCX2-EW-T07. The authors are indebted to the referee for the very valuable comments and his kind help in improving the clarity of the paper.

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© Springer Science+Business Media B.V. 2012

Authors and Affiliations

  • Jingxiu Wang
    • 1
  • Guiping Zhou
    • 1
  • Chunlan Jin
    • 1
  • Hui Li
    • 2
  1. 1.Key Laboratory of Solar Activity National Astronomical ObservatoriesChinese Academy of SciencesBeijingChina
  2. 2.Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of ScienceNanjingChina

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