Solar Physics

, Volume 114, Issue 2, pp 245–252 | Cite as

Spectral analysis and the two-dimensional distribution of physical parameters in a quiescent prominence

  • Q. Z. Zhang
  • W. C. Livingston
  • J. Hu
  • C. Fang
Article
Received:
Revised:

Abstract

The profiles of Hα and Ca ii K lines of a arch quiescent prominence on April 1, 1971 have been analyzed and the two-dimensional distributions of electron temperature T e , micro-turbulence velocity v t and the column number density of hydrogen along the line-of-sight NH have been obtained. T e , υ t , and N H are found to be 7500 K, 6 km s−1 and 2.2 × 1018 cm−2 on an average, respectively. The electron temperature at the central part of the prominence and along the two arcades are greater than that at the edges, while the distribution of the micro-turbulence velocity in these regions is opposite. There is no systematic variation in T e and v t , from the center to the periphery as described by Hirayama (1971). The column number density in the central region is lower than that at the two edges.

The contour lines of T e , υ t , and N H are predominantly vertical rather than horizontal. This implies that the height-variation of physical parameters in filamentary structure is small. The arrangement of this structure in the prominence is likely to be arched and is probably in the direction of magnetic field lines.

Keywords

Hydrogen Magnetic Field Central Region Spectral Analysis Physical Parameter 
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.
This is a preview of subscription content, log in to check access.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Engvold, O.: 1976, Solar Phys. 49, 283.Google Scholar
  2. Fang, C.: 1985, Publ. of Nanjing University (Science) 21, 10.Google Scholar
  3. Hirayama, T.: 1964, Publ. Astron. Soc. Japan 16, 104.Google Scholar
  4. Hirayama, T.: 1971, Solar Phys. 17, 50.Google Scholar
  5. Hirayama, T.: 1979, IAU Colloq. 44, 4.Google Scholar
  6. Hirayama, T.: 1985, Solar Phys. 100, 415.Google Scholar
  7. Hearn, A. G. and Holt, J. N.: 1973, Astron. Astrophys. 23, 347.Google Scholar
  8. Heasley, J. N. and Mihalas, D., 1976, Astrophys. J. 205, 273.Google Scholar
  9. Kavetsky, A. and O'Mara, B. J.: 1985, Solar Phys. 96, 1.Google Scholar
  10. Kavetsky, A. and O'Mara, B. J.: 1985,7. Quant. Spectr. Rad. Trans. 33, 93.Google Scholar
  11. Mouradian, Z. and Leroy, J. L.: 1977, Solar Phys. 51, 103.Google Scholar
  12. Wang, G. X. and Shi, Z. X.: 1983, Acta Astrophys. Sinica 3, 169.Google Scholar
  13. Yei, S. H.: 1961, Izv. Krymsk. Astrofiz. Obs. 25, 174.Google Scholar
  14. Zhang, Q. Z. and Fang, C.: 1986, Acta Astron. Sinica 27, 30.Google Scholar
  15. Zhang, Q. Z. and Fang, C.: 1987a, Acta Astrophys. Sinica 7, 133.Google Scholar
  16. Zhang, Q. Z. and Fang, C.: 1987b, Astron. Astrophys. 175, 277.Google Scholar

Copyright information

© Kluwer Academic Publishers 1987

Authors and Affiliations

  • Q. Z. Zhang
    • 1
  • W. C. Livingston
    • 2
  • J. Hu
    • 1
  • C. Fang
    • 1
  1. 1.Department of AstronomyNanjing UniversityNanjingChina
  2. 2.Kitt Peak National ObservatoryTucsonU.S.A.

Personalised recommendations