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Magnetic network elements in solar cycle 23

Published online by Cambridge University Press:  18 July 2013

Chunlan Jin  and
Jingxiu Wang
Chunlan Jin
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China. email: [email protected]
Jingxiu Wang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China. email: [email protected]
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Abstract

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In this report, we present our recent effort to understand the cyclic behavior of network magnetic elements based on the unique database from full-disk observations provided by Michelson Doppler Imager on board the Solar and Heliospheric Observatory in the interval including the entire cycle 23. The following results are unclosed. (1) The quiet regions dominate the solar magnetic flux for about 8 years in solar cycle 23, and from the solar minimum to maximum they contribute (0.94-1.44)×1023Mx flux to the solar photosphere. In the entire cycle 23, the magnetic flux of the quiet regions is 1.12 times that of active regions. The occupation ratio of quiet region flux equally characterizes the course of a solar cycle. (2) With the increasing magnetic flux per element, the variations of numbers and total flux of the network elements show three-fold scenario: no-correlation, anti-correlation, and correlation with sunspots, respectively. The anti-correlated elements covering the range of (3-32)×1018Mx occupy 77% of total element number and 37% of quiet Sun flux. (3) The time-latitude distribution of anti-correlated magnetic elements is out of phase with that of sunspots, while the correlated elements display the similar butterfly diagram of sunspots but with wider latitude distribution. These results imply that the correlated elements are the debris of decayed sunspots, and the source of anti-correlated elements is modulated by sunspot magnetic field.

Keywords

Sun: activitySun: dynamoSun: photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 131 - 136
Copyright
Copyright © International Astronomical Union 2013 

References

Davis, J. M. 1983, Sol. Phys., 88, 337 CrossRefGoogle Scholar
Davis, J. M., Golub, L., & Krieger, A. S. 1977, ApJ 214 L141. Google Scholar
Foukal, P., Harvey, K., & Hill, F. 1991, ApJ, 383, L89 CrossRefGoogle Scholar
Golub, L., Krieger, A. S., Harvey, J. W., & Vaiana, G. S. 1977, Sol. Phys., 53, 111 CrossRefGoogle Scholar
Golub, L., Davis, J. M., & Krieger, A. S. 1979, ApJ, 229, L145 CrossRefGoogle Scholar
Hagenaar, H. J., Schrijver, C. J., & Title, A. M. 2003, ApJ, 584, 1107 Google Scholar
Hara, H. & Nakakubo, K. 2003, ApJ, 589, 1062 Google Scholar
Harvey, J. 1971, Publ. Astron. Soc. Pacific, 83, 539 Google Scholar
Harvey, K. 1985, Aust. J. Phys., 38, 875 Google Scholar
Harvey, K. 1989, Bull. American Astron. Soc., 21, 839 Google Scholar
Harvey, K. & Harvey, J. 1974, Bull. American Astron. Soc., 6, 288 Google Scholar
Labonte, B. J. & Howard, R. 1982, Sol. Phys., 80, 15 CrossRefGoogle Scholar
Mehltretter, J. P. 1974, Sol. Phys., 38, 43 Google Scholar
Meunier, N. 2003, A&A, 405, 1107 Google Scholar
McIntosh, S W. & Gurman, J. B. 2005, Sol. Phys., 228, 285 CrossRefGoogle Scholar
Muller, R. & Roudier, T. 1984, Sol. Phys., 94, 33 Google Scholar
Muller, R. & Roudier, T. 1994, Sol. Phys., 152, 131 Google Scholar
Sattarov, I., Pevtsov, A. A., Hojaev, A. S., & Sherdonov, C. T. 2002, ApJ, 564, 1042 CrossRefGoogle Scholar
Sattarov, I., Pevtsov, A. A., Karachik, N. V., Sherdonov, C. T., & Tillaboev, A. M. 2010, Sol. Phys., 262, 321 Google Scholar
Sheeley, N. R. Jr. 1966, ApJ, 144, 723 Google Scholar
Sheeley, N. R. Jr. 1967, Sol. Phys., 1, 171 CrossRefGoogle Scholar
Trujillo Bueno, J., Shchukina, J. N. & Asensio Ramos, A. 2004, Nature, 430, 326 Google Scholar
White, O. R. & Livingston, W. C. 1981, ApJ, 249, 798 Google Scholar
Zirin, H. 1987, Sol. Phys., 110, 101 Google Scholar
Zhao, M., Wang, J. X., Jin, C. L., & Zhou, G. P. 2009, RAA, 9, 933 Google Scholar