Solar Physics

, Volume 156, Issue 2, pp 363–375 | Cite as

Simultaneous multifrequency observations of an eruptive prominence at millimeter wavelengths

  • Yoshihisa Irimajiri
  • Toshiaki Takano
  • Hiroshi Nakajima
  • Kiyoto Shibasaki
  • Yoichiro Hanaoka
  • Kiyoshi Ichimoto


Radio images and spectra of an eruptive prominence were obtained from simultaneous multifrequency observations at 36 GHz, 89 GHz, and 110 GHz on May 28, 1991 with the 45-m radio telescope at Nobeyama Radio Observatory (NRO), the National Astronomical Observatory, Japan (NAOJ). The radio spectra indicated that the optical depth is rather thick at 36 GHz whereas it is thin at 89 and 110 GHz. The Hα data, taken at Norikura Solar Observatory, NAOJ, suggest that the eruption of an active region filament was triggered by an Hα flare. The shape and position of the radio prominence generally coincided with those of Hα images. The radio emission is explained with an isothermal cool thread model. A lower limit for the electron temperature of the cool threads is estimated to be 6100 K. The range of the surface filling factors of the cool threads is 0.3–1.0 after the Hα flare, and 0.2–0.5 in the descending phase of the eruptive prominence. The column emission measure and the electron number density are estimated to be of the order of 1028 cm−5 and 1010 cm−3, respectively. The physical parameters of a quiescent prominence are also estimated from the observations. The filling factors of the eruptive prominence are smaller than those of the quiescent prominence, whereas the emission measures and the electron densities are similar. These facts imply that each cool thread of the prominence did not expand after the eruption, while the total volume of the prominence increased.


Filling Factor Emission Measure Radio Telescope Electron Number Density Radio Image 
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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  1. Apushkinsky, G. P. and Tsyganov, A. N.: 1972,Soln. Dann. No. 8, 100.Google Scholar
  2. Apushkinsky, G. P., Berulis, I. I., Losovskij, B. Ya., Sorochenko, R. L., Tsyganov, A. N., and Yasnov, L. V.: 1976,Soviet Astron. 20, 706.Google Scholar
  3. Butz, M, Fürst, E., Hirth, W., and Kundu, M. R.: 1975,Solar Phys. 45, 125.Google Scholar
  4. Chiuderi-Drago, F.: 1989, in V. Ruždjak and E. Tandberg-Hanssen (eds.), ‘Dynamics of Quiescent Prominences’,Proc. IAU Colloq. 117, 70.Google Scholar
  5. Chiuderi-Drago, F., Engvold, O., and Jensen, E.: 1992,Solar Phys. 139, 47.Google Scholar
  6. Demoulin, P., Raadu, M. A., Malherbe, J. M., and Schmieder, B.: 1987,Astron. Astrophys. 183, 142.Google Scholar
  7. Engvold, O.: 1976,Solar Phys. 49, 283.Google Scholar
  8. Hanaoka, Y., Kurokawa, H., Enome, S., Nakajima, H., Shibasaki, K., Nishio, M., Takano, T., Torii, C., Sekiguchi, H., Kawashima, S., Bushimata, T., Shinohara, N., Irimajiri, Y., Koshiishi, H., Shiomi, Y., Nakai, Y., Funakoshi, Y., Kitai, R., Ishiura, K., and Kimura, G.: 1994,Publ. Astron. Soc. Japan 46, 205.Google Scholar
  9. Hirayama, T.: 1985,Solar Phys. 100, 415.Google Scholar
  10. Ichimoto, K., Sakurai, T., Yamaguchi, A., Kumagai, K., Nishino, Y., Suematsu, Y., Hiei, E., and Hirayama, T.: 1991, in Y. Uchida, R. C. Canfield, T. Watanabe, and E. Hiei (eds.),Flare Physics in Solar Activity Maximum 22, LectureNotes in Physics 387, 320.Google Scholar
  11. Irimajiri, Y. and Takano, T.: 1991,Exper. Astron. 2(2), 123.Google Scholar
  12. Irimajiri, Y., Takano, T., and Tokumaru, M.: 1988,IEICE Japan, Tech. Report AP88–95, 27.Google Scholar
  13. Irimajiri, Y., Takano, T., and Tokumaru, M.: 1990,IEICE Japan, Trans. J73-BII, 20.Google Scholar
  14. Kosugi, T., Ishiguro, M., and Shibasaki, K.: 1986,Publ. Astron. Soc. Japan 38, 1.Google Scholar
  15. Kundu, M. R.: 1972,Solar Phys. 25, 108.Google Scholar
  16. Kundu, M. R. and Lantos, P.: 1977,Solar Phys. 52, 393.Google Scholar
  17. Kundu, M. R., Fürst, E., Hirth., W., and Butz, M.: 1978,Astron. Astrophys. 62, 431.Google Scholar
  18. Linsky, J. L.: 1973,Solar Phys. 28, 409.Google Scholar
  19. Orrall, F. Q. and Schmahl, E. J.: 1976,Solar Phys. 50, 365.Google Scholar
  20. Orrall, F. Q. and Schmahl, E. J.: 1980,Astrophys. J. 240, 908.Google Scholar
  21. Poland, A. I. and Munro, H.: 1976,Astrophys. J. 209, 927.Google Scholar
  22. Priest, E.R. (ed.): 1989,Dynamics and Structure of Quiescent Prominences, Kluwer Academic Publishers, Dordrecht, Holland, Ch. 1, p. 1.Google Scholar
  23. Rao, A. P. and Kundu, M. R.: 1977,Solar Phys. 55, 161.Google Scholar
  24. Raoult, A., Lantos, P., and Fürst, E.: 1979,Solar Phys. 61, 335.Google Scholar
  25. Schmahl, E. and Hildner, E.: 1977,Solar Phys. 55, 473.Google Scholar
  26. Simon, M. and Wickstrom, B. A.: 1971,Solar Phys. 20, 122.Google Scholar
  27. Smith, J. B., Speich, D. M. and Wu, S. T.: 1977,Solar Phys. 52, 379.Google Scholar
  28. Takano, T. and Irimajiri, Y.: 1994,Astron. Astrophys., submitted.Google Scholar
  29. Zodi, A. M., Correia, E., Costa, J. E. R., Kaufmann, P., Martin, S. F., and Kundu, M. R.: 1988,Solar Phys. 116, 83.Google Scholar

Copyright information

© Kluwer Academic Publishers 1995

Authors and Affiliations

  • Yoshihisa Irimajiri
    • 1
  • Toshiaki Takano
    • 1
  • Hiroshi Nakajima
    • 1
  • Kiyoto Shibasaki
    • 1
  • Yoichiro Hanaoka
    • 1
  • Kiyoshi Ichimoto
    • 2
  1. 1.Nobeyama Radio Observatory, The National Astronomical ObservatoryNaganoJapan
  2. 2.The National Astronomical ObservatoryTokyoJapan

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