Solar Physics

, Volume 132, Issue 1, pp 63–80 | Cite as

Structure and oscillations in quiescent filaments from observations in He i λ10830 å

  • Yi Zhang
  • Oddbjørn Engvold
  • Stephen L. Keil


Observations of two quiescent filaments show oscillatory variations in Doppler shift and central intensity of the He i λ10830 Å line.

The oscillatory periods range from about 5 to 15 min, with dominant periods of 5, 9, and 16 min. The 5-min period is also detected in the intensity variations, after correction for atmospheric effects. Doppler shifts precede intensity variations by about one period. The possibility that the oscillations are Alfvén waves is discussed.

The Doppler signals of the filament form fibril-like structures. The fibrils are all inclined at an angle of about 25° to the long axis of the filament. The magnetic field has a similar orientation relative to the major direction of the filament, and the measured Doppler signals are apparently produced by motions along magnetic flux tubes threading the filament.

The measured lifetimes of the small-scale fibrils of quiescent disk filaments are very likely a combined effect of intensity modulations and reshuffling of the structures.


Fibril Magnetic Flux Intensity Variation Doppler Shift Filament Form 
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.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Balthasar, H., Knölker, M., Stellmacher, G., and Wiehr, E.: 1986, Astron. Astrophys. 163, 343.Google Scholar
  2. Bahskirtsev, V. S. and Mashnich, G. P.: 1984, Solar Phys. 91, 93.Google Scholar
  3. Breckinridge, J. B. and Hall, D. N. B.: 1973, Solar Phys, 28, 15.Google Scholar
  4. Demoulin, P., Raadu, M. A., Malherbe, J. M., and Schmieder, B.: 1987, Astron. Astrophys. 183, 142.Google Scholar
  5. Dunn, R. B.: 1960, Ph.D. Thesis, Harvard University.Google Scholar
  6. Dunn, R. B.: 1969, Sky Telesc 38, 368.Google Scholar
  7. Engvold, O.: 1976, Solar Phys. 49, 283.Google Scholar
  8. Engvold, O.: 1978, Solar Phys. 56, 87.Google Scholar
  9. Engvold, O., Malville, J. M., and Livingston, W.: 1978, Solar Phys. 60, 57.Google Scholar
  10. Engvold, O., Hirayama, T., Leroy, J.-L., Priest, E. R., and Tandberg-Hanssen, E.: 1989, in V. Ruždjak and E. Tandberg-Hanssen (eds.), Proc. IAU Colloq. 119.Google Scholar
  11. Ghenojian, L. A., Klepikov, V. Yu., and Stepanov, A. I.: 1990, Academy of Sciences of the USSR, IZIMIRAN, Reprint No. 4.Google Scholar
  12. Giovanelli, R. G., Hall, D. N. B., and Harvey, J. W.: 1972, Solar Phys. 22, 53.Google Scholar
  13. Golub, L.: 1976, Solar Phys. 46, 115.Google Scholar
  14. Heasley, J. N. and Milkey, R. W.: 1976, Astrophys. J. 210, 827.Google Scholar
  15. Hollweg, J. V.: 1971, J. Geophys. Res. 76, 5155.Google Scholar
  16. Jensen, E.: 1983, Solar Phys. 89, 275.Google Scholar
  17. Jensen, E.: 1989, in ‘Dynamics of Prominences’, V. Ruždjak and E. Tandberg-Hanssen (eds.), Proc. IAU Colloq. 119.Google Scholar
  18. Kim, I. S.: 1990, ‘Prominence Magnetic Field Observations’, Preprint 11 from GAIS, Sternberg State Astronomical Institute, Moscow State University.Google Scholar
  19. Labs, D. and Neckel, H.: 1970, Solar Phys. 15, 79.Google Scholar
  20. Labs, D. and Neckel, H.: 1973, Proceedings of Symposium on Solar Radiation, Smithsonian Institution, Washington, D.C., 269.Google Scholar
  21. Leroy, J. L., Bommier, V., and Sahal-Brechot, S.: 1983, Solar Phys. 83, 135.Google Scholar
  22. Leroy, J. L., Bommier, V., and Sahal-Brechot, S.: 1983, Astron. Astrophys. 131, 33.Google Scholar
  23. Malherbe, J. M., Schmieder, B., and Mein, P.: 1981, Astron. Astrophys. 55, 103.Google Scholar
  24. Malherbe, J. M., Schmieder, B., Mein, P., and Tandberg-Hanssen, E.: 1987, Astron. Astrophys. 172, 316.Google Scholar
  25. Malville, J. M. and Schindler, M.: 1981, Solar Phys. 70, 115.Google Scholar
  26. Milkey, R. W., Heasley, J. N., Schmahl, E. J., and Engvold, O.: 1978, in E. Jensen, P. Maltby, and F. Orrall (eds.), ‘Physics of Solar Prominences’ IAU Colloq. 44, 53.Google Scholar
  27. Simon, G., Schmieder, B., Demoulin, P., and Poland, A. I.: 1986, Astron. Astrophys. 166, 319.Google Scholar
  28. Solov'ev, A. A.: 1985, Soln. Dannye No. 9, 65.Google Scholar
  29. Suematsu, Y., Yoshinaga, R., Terao, N., and Tsubaki, T.: 1990, Publ. Astron. Soc. Japan 42, 187.Google Scholar
  30. Tandberg-Hanssen, E. and Anzer, U.: 1970, Solar Phys. 15, 158.Google Scholar
  31. Tsubaki, T. and Takeuchi, A.: 1986, Solar Phys. 104, 313.Google Scholar
  32. Tsubaki, T., Ohnishi, Y., and Suematsu, Y.: 1987, Publ. Astron. Soc. Japan 39, 179.Google Scholar
  33. Tsubaki, T., Toyoda, M., Suematsu, Y., and Gamboa, G. A. R.: 1988, Publ. Astron. Soc. Japan 40, 121.Google Scholar
  34. Uchida, Y.: 1980, in F. Moriyama and J. C. Hénoux (eds.), Proceedings of ‘The Japan-France Seminar on Solar Physics’, p. 169.Google Scholar
  35. Vial, J. C.: 1982, Astrophys. J. 254, 780.Google Scholar
  36. Wiehr, E., Stellmacher, G., and Balthasar, H.: 1984, Solar Phys. 94, 285.Google Scholar
  37. Yakovkin, N. A. and Zel-dina, M. Yu.: 1964, Soviet Astron.-AJ 7, 643.Google Scholar
  38. Yi Zhang, Engvold, O., and Jensen, E.: 1991, in preparation.Google Scholar

Copyright information

© Kluwer Academic Publishers 1991

Authors and Affiliations

  • Yi Zhang
    • 1
  • Oddbjørn Engvold
    • 1
  • Stephen L. Keil
    • 2
  1. 1.Institute of Theoretical AstrophysicsUniversity of OsloBlindernNorway
  2. 2.AFGLSunspotU.S.A.

Personalised recommendations