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Astrophysics and Space Science

, Volume 181, Issue 1, pp 111–115 | Cite as

The distribution of sunspots over the Sun

  • Wahab Uddin
  • M. C. Pande
  • V. K. Verma
Article

Abstract

The distribution of the sunspots for the period 1967–1987 (solar cycles 20 and 21) is presented here. We find that the ±11–20° latitude belt is most prolific for the occurrence of various spot types irrespective of magnetic-field ranges. Furthermore, longitudinally sunspots occur most prolifically at six or more places on the Sun. Spatially 7–9 zones are present in each hemisphere (north or south) of the Sun where about 50% sunspots occur and occupy only about 4% area of the Sun. During the above cycles at least 5 flare zones were regularly present in each hemisphere. The existing models cannot explain these active zones on the Sun. Thus, the present analysis emphasizes the need for a new magnetic models of the Sun.

Keywords

Flare Solar Cycle Active Zone Magnetic Model Latitude Belt 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. Babcock, H. W.: 1961,Astrophys. J. 133, 572.Google Scholar
  2. Carrington, R. C.: 1958,Montly Notices Roy. Astron. Soc. 19, 1.Google Scholar
  3. Gnevyshev, M. N.: 1938,Pulkovo Obs. Circ. 24, 37.Google Scholar
  4. Kopecký, M.: 1960,Bull. Astron. Inst. Czech.,11, 35.Google Scholar
  5. Kopecký, M. and Kopecká, F.: 1984,Bull. Astron. Inst. Czech. 35, 233.Google Scholar
  6. Kozhevnikov, N. I.: 1970,Soob. Gos. Astron. Inst. Shternberg, No. 162, p. 16.Google Scholar
  7. Kuklin, G. V.: 1962,Soln. Dann. No. 1, p. 72.Google Scholar
  8. Maris, G.: 1972,Stud. Sci. Circ. Astron. 17, 71.Google Scholar
  9. Maunder, E. W.: 1922,Stud. Sci. Circ. Astron. 82, 534.Google Scholar
  10. Morozov, N. N. and Obashev, S. O.: 1969,Tr. Astrofiz. Inst. Akad. Nauk Kaz SSR 15, 38.Google Scholar
  11. Morozov, N. N., Obashev, S. O., and Beshenov, G.: 1973,Tr. Astrofiz Inst. Alma-Ata 23, 48.Google Scholar
  12. Ozguc, A. and Duzgelen, A.: 1989,Astrophys. Space Sci. 162, 27.Google Scholar
  13. Parker, E. N.: 1955,Astrophys. J. 122, 293.Google Scholar
  14. Shelke, R. N. and Verma, V. K.: 1985,Bull. Astron. Soc. India 13, 53.Google Scholar
  15. Smith, S. F. and Howard, R.: 1967, in K. O. Kiepenheuer (ed.), ‘Structure and Development of Solar Active Regions’,IAU Symp. 35, 33.Google Scholar
  16. Trellis, M.: 1971a,Compt. Rend. Acad. Sci. 272, B549.Google Scholar
  17. Trellis, M.: 1971b,Compt. Rend. Acad. Sci. 272, B1026.Google Scholar
  18. Verma, V. K. and Pande, M. C.: 1988,Indian J. Rad. Sp. Phys. 17, 8.Google Scholar
  19. Verma, V. K., Pande, M. C., and Uddin, W.: 1987,Solar Phys. 112, 341.Google Scholar
  20. Vitinsky, Yu. I.: 1969,Solar Phys. 7, 210.Google Scholar
  21. Warwick, C. S.: 1965,Astrophys. J. 141, 50.Google Scholar

Copyright information

© Kluwer Academic Publishers 1991

Authors and Affiliations

  • Wahab Uddin
    • 1
  • M. C. Pande
    • 1
  • V. K. Verma
    • 1
  1. 1.Uttar Pradesh State ObservatoryNaini TalIndia

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