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Astronomy Letters

, Volume 40, Issue 8, pp 510–518 | Cite as

Investigation of the evolution of coronal bright points and magnetic field topology

  • E. P. MinenkoEmail author
  • N. V. Karachik
  • I. Sattarov
  • A. A. Pevtsov
Article

Abstract

Our investigation has been carried using the instruments onboard the Solar Dynamics Observatory (SDO) providing a high resolution of images (AIA photographs and HMI magnetograms). We have investigated the structure and magnetic evolution of several coronal bright points and small scale N-S polarity magnetic fluxes closely associated with them. We also compare the evolution of the magnetic polarities of elementary isolated sources of positive and negative fluxes (magnetic bipoles) and coronal bright points. Tiny (“elementary”) coronal bright points have been detected. A standard coronal bright point is shown to be a group of “elementary” coronal bright points that flare up sequentially. Our investigation shows that a change in the magnetic fluxes of opposite polarities is observed before the flare of a coronal bright point. We show that not all cases of the formation of coronal bright points are described by the magnetic reconnection model. This result has not been considered previously and has not been pointed out by other authors.

Keywords

Sun coronal bright points magnetic field 

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References

  1. 1.
    J. W. Cirtain, L. Golub, L. Lundquist, A. van Ballegooijen, A. Savcheva, M. Shimojo, E. DeLuca, S. Tsuneta, T. Sakao, K. Reeves, M. Weber, R. Kano, N. Narukage, and K. Shibasaki, Science 318, 1580 (2007).ADSCrossRefGoogle Scholar
  2. 2.
    E. N. Frazier, Solar Phys. 26, 130 (1972).ADSCrossRefGoogle Scholar
  3. 3.
    L. Golub, A. S. Krieger, J. W. Harvey, and G. S. Vaiana, Solar Phys. 53, 111 (1977).ADSCrossRefGoogle Scholar
  4. 4.
    L. Golub, A. S. Krieger, J. K. Silk, A. F. Timothy, and G. S. Vaiana, Astrophys. J. 189, L93 (1974).ADSCrossRefGoogle Scholar
  5. 5.
    H. Hara and K. Nakakubo-Morimoto, Astrophys. J. 589, 1062 (2003).ADSCrossRefGoogle Scholar
  6. 6.
    K. L. Harvey, Austral. J. Phys. 38, 875 (1985).ADSCrossRefGoogle Scholar
  7. 7.
    K. L. Harvey, J. W. Harvey and S. F. Martin, Solar Phys. 40, 87 (1975).ADSGoogle Scholar
  8. 8.
    Y. Jiang, Y. Bi, J. Yang, H. Li, B. Yang, and R. Zheng, Astrophys. J. 775, 132 (2013).ADSCrossRefGoogle Scholar
  9. 9.
    R. Kariyappa, E. E. Deluca, S. H. Saar, L. Golub, L. Dam’e, A. A. Pevtsov, and B. A. Varghese, Astron. Astrophys. 526, A78 (2011).ADSCrossRefGoogle Scholar
  10. 10.
    Y. Liu, J. T. Hoeksema, P. H. Scherrer, J. Schou, S. Couvidat, R. I. Bush, T. L. Duvall, K. Hayashi, X. Sun, and X. Zhao, Solar Phys. 279, 295 (2012).ADSCrossRefGoogle Scholar
  11. 11.
    D.W. Longcope, Astrophys. J. 507, 433 (1998).ADSCrossRefGoogle Scholar
  12. 12.
    D. W. Longcope and C. C. Kankelborg, Astrophys. J. 524, 483 (1999).ADSCrossRefGoogle Scholar
  13. 13.
    D.W. Longcope, C. C. Kankelborg, J. L. Nelson, and A. A. Pevtsov, Astrophys. J. 553, 429 (2001).ADSCrossRefGoogle Scholar
  14. 14.
    S.W. McIntosh and J. B. Gurman, Solar Phys. 228, 285 (2005).ADSCrossRefGoogle Scholar
  15. 15.
    R. L. Moore, A. C. Sterling, J. W. Cirtain, and D. A. Falconer, Astrophys. J. 731, L18 (2011).ADSCrossRefGoogle Scholar
  16. 16.
    K. Nakakubo and H. Hara, Adv. Space Res. 25, 1905 (2000).ADSCrossRefGoogle Scholar
  17. 17.
    J. L. Nelson, D.W. Longcope, and A. A. Pevtsov, Bull. Am. Astron. Soc. 32, 1289 (2000).ADSGoogle Scholar
  18. 18.
    W. D. Pesnell, B. J. Thompson, and P. C. Chamberlin, Solar Phys. 275, 3 (2012).ADSCrossRefGoogle Scholar
  19. 19.
    E. R. Priest, C. E. Parnell, and S. F. Martin, Astrophys. J. 427, 459 (1994).ADSCrossRefGoogle Scholar
  20. 20.
    I. Sattarov, A. A. Pevtsov, A. S. Hojaev, and C. T. Sherdonov, Astrophys. J. 564, 1042 (2002).ADSCrossRefGoogle Scholar
  21. 21.
    I. Sattarov, A. A. Pevtsov, N. V. Karachek, and C. T. Sherdanov, Multi-Wavelength Invest. Solar Activ. 223, 667 (2004).ADSGoogle Scholar
  22. 22.
    I. Sattarov, A. A. Pevtsov, N. V. Karachik, and B. J. Sattarova, Large-Scale Struct. Their Role Solar Activ. 346, 395 (2005a).ADSGoogle Scholar
  23. 23.
    I. Sattarov, A. A. Pevtsov, N. V. Karachik, and B. J. Sattarova, Large-Scale Struct. Their Role Solar Activ. 346, 363 (2005b).ADSGoogle Scholar
  24. 24.
    I. Sattarov, A. A. Pevtsov, N. V. Karachik, C. T. Sherdanov, and A. M. Tillaboev, Solar Phys. 262, 321 (2010).ADSCrossRefGoogle Scholar
  25. 25.
    C. T. Sherdanov, E. P. Minenko, A. M. Tillaboev, and I. Sattarov, Astrophys. Space Sci. Proc. 30, 197 (2012).CrossRefGoogle Scholar
  26. 26.
    L. P. van Speybroeck, A. S. Krieger, and G. S. Vaiana, Nature 227, 818 (1970).ADSCrossRefGoogle Scholar
  27. 27.
    K. Ueda, R. Kano, S. Tsuneta, and H. Shibahashi, Solar Phys. 261, 77 (2010).ADSCrossRefGoogle Scholar
  28. 28.
    J. Warnecke, I. R. Losada, A. Brandenburg, N. Kleeorin, and I. Rogachevskii, Astrophys. J. 777, L37 (2013).ADSCrossRefGoogle Scholar
  29. 29.
    S. F. Webb, D. F. Martin, D. Moses, and J.W. Harvey, Solar Phys. 144, 15 (1993).ADSCrossRefGoogle Scholar
  30. 30.
    K. Yoshimura, ASP Conf. Ser. 454, 245 (2012).ADSGoogle Scholar
  31. 31.
    Q.M. Zhang and H. S. Ji, Astron. Astrophys. 557, L5 (2013).ADSCrossRefGoogle Scholar

Copyright information

© Pleiades Publishing, Inc. 2014

Authors and Affiliations

  • E. P. Minenko
    • 1
    Email author
  • N. V. Karachik
    • 2
  • I. Sattarov
    • 2
  • A. A. Pevtsov
    • 3
  1. 1.Ulugh Beg Astronomical InstituteAcademy of Sciences of UzbekistanTashkentUzbekistan
  2. 2.Tashkent State Pedagogical UniversityTashkentUzbekistan
  3. 3.National Solar Observatory, Sacramento PeakSunspotUSA

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