Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-25T04:38:04.318Z Has data issue: false hasContentIssue false
  • English
  • Français

Are there local dynamo in solar polar region?

Published online by Cambridge University Press:  24 September 2020

Chunlan Jin Open the ORCID record for Chunlan Jin [Opens in a new window]
Chunlan Jin*
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing100101, China email: mailto:[email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Polar magnetic field, as a component produced by the global dynamo, is thought to be the remant of toroidal magnetic field transported poleward from Sun’s active belt. With the improvement of instruments, more and more observations are challenging the viewpoint. Recently, we identify the bipolar magnetic emergences (BMEs) in the polar region, and find that the distribution of the magnetic axes for these BMEs shows random state, which does not follow the Joy’s law of active region. The result implies the possible existence of local dynamo in the solar polar region.

Keywords

Sun: atmosphereSun: magnetic fieldsSun: photospheresunspots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 123 - 126
Copyright
© International Astronomical Union 2020

References

Babcock, H. W. & Babcock, H. D. 1955, Astrophys. J., 121, 349CrossRefGoogle Scholar
Benevolenskaya, E. E. 2004, A&A, 428, L5Google Scholar
Deng, Y. Y., Wang, J. X., & Ai, G. X. 1999, Science in China, 42, 10Google Scholar
Ito, H., Tsuneta, S., Shiota, D., Tokumaru, M., & Fujiki, K. 2010, Astrophys. J., 719, 131CrossRefGoogle Scholar
Jin, C. L. & Wang, J. X. 2011, Astrophys. J., 732, 4CrossRefGoogle Scholar
Jin, C. L., Zhou, G. P., Zhang, Y. Z., & Wang, J. X. 2020, Astrophys. J. Lett., 889, L26CrossRefGoogle Scholar
Lin, H., Varsik, J., & Zirin, H. 1994, Sol. Phys., 155, 243CrossRefGoogle Scholar
Severny, A. B. 1971, IAUS, 43, 675Google Scholar
Sheeley, N. R., Jr. 1992, ASPC, 27, 1Google Scholar
Sheeley, N. R., Jr. 2005, LRSP, 2, 5Google Scholar
Shiota, D., Tsuneta, S., Shimojo, M., Sako, N., et al. 2012, Astrophys. J., 753, 157CrossRefGoogle Scholar
Sun, X., Hoeksema, J. T., Liu, Y., Norton, A. A., et al. 2015, American Geophysical Union, Fall Meeting, SH23A-2429Google Scholar
Tang, F. & Wang, H. M. 1991, Sol. Phys., 132, 247CrossRefGoogle Scholar
Tsuneta, S., Ichimoto, K., Katsukawa, Y., Lites, B. W., et al. 2008, Astrophys. J., 688, 1374CrossRefGoogle Scholar
Wang, Y. M., Sheeley, N. R., Jr., & Nash, A. G. 1991, Astrophys. J., 383, 431CrossRefGoogle Scholar