Advertisement

Solar Physics

, Volume 283, Issue 2, pp 273–282 | Cite as

Solar Intranetwork Magnetic Elements: Flux Distributions

  • Guiping Zhou
  • Jingxiu Wang
  • Chunlan Jin
Article
First Online:
Received:
Accepted:

Abstract

The current study aims at quantifying the flux distributions of solar intranetwork (IN) magnetic field based on the data taken in four quiet and two enhanced network areas with the Narrow-band Filter Imager of the Solar Optical Telescope on board the Hinode satellite. More than 14000 IN elements and 3000 NT elements were visually identified. They exhibit a flux distribution function with a peak at 1 – 3×1016 Mx (maxwell) and 2 – 3×1017 Mx, respectively. We found that the IN elements contribute approximately to 52 % of the total flux and an average flux density of 12.4 gauss of the quiet region at any given time. By taking the lifetime of IN elements of about 3 min (Zhou et al., Solar Phys. 267, 63, 2010) into account, the IN fields are estimated to have total contributions to the solar magnetic flux up to 3.8×1026 Mx per day. No fundamental distinction can be identified in IN fields between the quiet and enhanced network areas.

Keywords

Magnetic fields Photosphere 
This is a preview of subscription content, log in to check access.

Notes

Acknowledgements

We sincerely thank Professor Sakurai, Editor in Chief of Solar Physics, for his very careful corrections and great improvements. We also thank the anonymous referees for their constructive comments and suggestions. We are grateful to all members of Hinode teams for providing the wonderful 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. The work is supported by the National Natural Science Foundation of China (10973019, 11003024, 10873020, 40731056, 40890161, 40974112, 11025315, 11003026, 10873038, 10833007 and 10921303), the Chinese Academy of Science Project KJCX2-EW-T07, and the National Key Basic Research Science Foundation (G2011CB811403 and G2011CB811402).

References

  1. Bommier, V., Landi Degl’ Innocenti, E., Landolfi, M., Molodij, G.: 2007, In: Demircan, O., Selam, S.O., Albayrak, B. (eds.) Solar and Stellar Physics through Eclipses, ASP Conf. Ser. 370, 81. Google Scholar
  2. Domínguez Cerdeña, I., Sánchez Almeida, J., Kneer, F.: 2003, Astron. Astrophys. 407, 741. ADSCrossRefGoogle Scholar
  3. Domínguez Cerdeña, I., Sánchez Almeida, J., Kneer, F.: 2006, Astrophys. J. 636, 496. ADSCrossRefGoogle Scholar
  4. Hagenaar, H.J., Schrijver, C.J., Title, A.M.: 2003, Astrophys. J. 584, 1107. ADSCrossRefGoogle Scholar
  5. Hartj, B., Kneer, F.: 2002, Astron. Astrophys. 385, 264. ADSCrossRefGoogle Scholar
  6. Ichimoto, K., Lites, B., Elmore, D., Suematsu, Y., Tsuneta, S., Katsukawa, Y., et al.: 2008, Solar Phys. 249, 233. ADSCrossRefGoogle Scholar
  7. Jin, C.L., Wang, J.X., Xie, Z.X.: 2012, Solar Phys. 280, 51. ADSCrossRefGoogle Scholar
  8. Khomenko, E., Collados, M.: 2006, In: Casini, R., Lites, B.W. (eds.) Solar Polarization 4, ASP Conf. Ser. 358, 42. Google Scholar
  9. Khomenko, E.V., Collados, M., Solanki, S.K., Lagg, A., Trujillo Bueno, J.: 2003, Astrophys. J. 408, 1115. ADSGoogle Scholar
  10. Khomenko, E.V., Martínez González, M.J., Collados, M., Vögler, A., Solanki, S.K., Ruiz Cobo, B., Beck, C.: 2005, Astron. Astrophys. 436, 27. ADSCrossRefGoogle Scholar
  11. Kosugi, T., Matsuzaki, K., Sakao, T., Shimizu, T., Sone, Y., Tachikawa, S., et al.: 2007, Solar Phys. 243, 3. ADSCrossRefGoogle Scholar
  12. Lin, H., Rimmele, T.: 1999, Astrophys. J. 514, 448. ADSCrossRefGoogle Scholar
  13. Lites, B.W.: 2002, Astrophys. J. 573, 431. ADSCrossRefGoogle Scholar
  14. Lites, B.W., Kubo, M., Socas-Navarro, H., Berger, T., Frank, Z., Shine, R., et al.: 2008, Astrophys. J. 672, 1237. ADSCrossRefGoogle Scholar
  15. Meunier, N., Solanki, S.K., Livingston, W.C.: 1998, Astron. Astrophys. 331, 771. ADSGoogle Scholar
  16. Parker, E.N.: 1991, Astrophys. J. 372, 719. ADSCrossRefGoogle Scholar
  17. Parnell, C.E., Jupp, P.E.: 2000, Astrophys. J. 529, 554. ADSCrossRefGoogle Scholar
  18. Parnell, C.E., DeForest, C.E., Hagenaar, H.J., Johnston, B.A., Lamb, D.A., Welsch, B.T.: 2009, Astrophys. J. 698, 75. ADSCrossRefGoogle Scholar
  19. Sánchez Almeida, J.: 2003, Astron. Astrophys. 411, 615. ADSCrossRefGoogle Scholar
  20. Sánchez Almeida, J., Lites, B.W.: 2000, Astrophys. J. 532, 1215. ADSCrossRefGoogle Scholar
  21. Schüssler, M.: 2007, Astron. Nachr. 328, 1087. ADSCrossRefGoogle Scholar
  22. Shimizu, T., Nagata, S., Tsuneta, S., Tarbell, T., Edwards, C., Shine, R., et al.: 2008, Solar Phys. 249, 221. ADSCrossRefGoogle Scholar
  23. Socas-Navarro, H., Martínez Pillet, V., Lites, B.W.: 2004, Astrophys. J. 611, 1139. ADSCrossRefGoogle Scholar
  24. Suematsu, Y., Tsuneta, S., Ichimoto, K., Shimizu, T., Otsubo, M., Katsukawa, Y., et al.: 2008, Solar Phys. 249, 197. ADSCrossRefGoogle Scholar
  25. Trujillo Bueno, J., Shchukina, N., Asensio Ramos, A.: 2004, Nature 430, 326. ADSCrossRefGoogle Scholar
  26. Tsuneta, S., Ichimoto, K., Katsukawa, Y., Nagata, S., Otsubo, M., Shimizu, T., et al.: 2008, Solar Phys. 249, 167. ADSCrossRefGoogle Scholar
  27. Vögler, A., Shelyag, S., Schüssler, M., Cattaneo, F., Emonet, T., Linde, T.: 2005, Astron. Astrophys. 429, 335. ADSCrossRefGoogle Scholar
  28. Wang, J., Zirin, H., Shi, Z.: 1985, Solar Phys. 98, 241. ADSCrossRefGoogle Scholar
  29. Wang, J., Wang, H., Tang, F., Lee, J.W., Zirin, H.: 1995, Solar Phys. 160, 277. ADSCrossRefGoogle Scholar
  30. Wang, J., Zhou, G.P., Jin, C.L., Li, H.: 2012, Solar Phys. 278, 299. ADSCrossRefGoogle Scholar
  31. Zhao, M., Wang, J.X., Jin, C.L., Zhou, G.: 2009, Res. Astron. Astrophys. 9, 933. ADSCrossRefGoogle Scholar
  32. Zhou, G.P., Wang, J.X., Jin, C.L.: 2010, Solar Phys. 267, 63. ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 2013

Authors and Affiliations

  1. 1.Key Laboratory of Solar Activity, National Astronomical ObservatoriesChinese Academy of SciencesBeijingChina

Personalised recommendations

Cite article

Buy options