Solar Physics

, Volume 183, Issue 1, pp 107–121 | Cite as

Neutral Hydrogen Column Depths in Prominences Using EUV Absorption Features

  • T.A. Kucera
  • V. Andretta
  • A.I. Poland


Observations of prominence regions in hot coronal lines (≳106 K) at wavelengths below the hydrogen Lyman absorption limit show what appear to be absorption features. Other authors have suggested that these observed features may be due to H and He continuum absorption. But there has, as yet, been no conclusive evidence that this is indeed the case. In this paper we present new Solar and Heliospheric Observatory (SOHO) observations that allow us to address this problem in a quantitative manner. We find that continuum absorption is the best explanation for the absorption observed in imaging data from the Coronal Diagnostic Spectrometer (CDS) on board SOHO. Furthermore, we discuss a new technique to measure the column depth of neutral hydrogen in a prominence, and use it to obtain estimates of the prominence filling factors as well. We calculate the column depth of neutral hydrogen, ξH∼1018 cm−2, and the filling factor, f≳0.3.


Hydrogen Imaging Data Absorption Feature Filling Factor Good Explanation 
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. Arnaud, M. and Rothenflug, R.: 1985, Astron. Astrophys. Suppl. Ser. 60, 425.Google Scholar
  2. Batchelor, D. A. and Schmahl, E. J.: 1994, Proc. of the Third SOHO Workshop, ESA SP-373, p. 203.Google Scholar
  3. Engvold, O.: 1989, in E. R. Priest, (ed.), Dynamics and Structure of Quiescent Solar Prominences, Kluwer Academic Publishers, Dordrecht, Holland, p. 47.Google Scholar
  4. Fernley, J. A., Taylor, K. T., and Seaton, M. J.: 1987, J. Phys. B20, 6457.Google Scholar
  5. Harrison, R. A. et al.: 1996, Solar Phys. 162, 233.Google Scholar
  6. Heinzel, P., Bommier, V., and Vial, J. C.: 1996, Solar Phys. 164, 211.Google Scholar
  7. Hirayama, T.: 1989, in V. Ruždjak and E. Tandberg-Hanssen (eds.), Dynamics of Quiescent Prominences, Springer-Verlag, Berlin, p. 187.Google Scholar
  8. Karzas, W. J. and Latter, R.: 1961, Astrophys. J. Suppl. Ser. 6, 167.Google Scholar
  9. Landman, D. A.: 1984, Astrophys. J. 279, 438.Google Scholar
  10. Landman, D. A.: 1986, Astrophys. J. 305, 546.Google Scholar
  11. Martens, P. C. H., Van der Oord, G. H. J., and Hoyng, P.: 1985, Solar Phys. 96, 253.Google Scholar
  12. Orrall, F. Q. and Schmahl, E. J.: 1976, Solar Phys. 50, 365.Google Scholar
  13. Smartt, R. N. and Zhang, Z.: 1984, Solar Phys. 90, 315.Google Scholar
  14. Stellmacher, G. and Wiehr, E.: 1997, Astron. Astrophys. 319, 669.Google Scholar
  15. Thompson, W.: 1997, CDS Software Note, No. 49, ver. 3.Google Scholar
  16. West, J. B. and Marr, G. V.: 1976, Proc. Roy. Soc. London A349, 397.Google Scholar

Copyright information

© Kluwer Academic Publishers 1998

Authors and Affiliations

  • T.A. Kucera
    • 1
  • V. Andretta
    • 2
  • A.I. Poland
    • 1
  1. 1.NASA/GSFCLaboratory for Astronomy and Solar Physics, Code 682.3GreenbeltU.S.A.
  2. 2.NASA/GSFCLaboratory for Astronomy and Solar Physics, Code 682.3GreenbeltU.S.A.

Personalised recommendations