Solar Physics

, Volume 226, Issue 1, pp 3–16 | Cite as

Differentiating Coronal Holes from the Quiet Sun by He 1083 nm Imaging Spectroscopy



The locations of coronal holes are usually based on equivalent-width images in the He i 1083 nm line. However, it is difficult to differentiate coronal holes from the centers of quiet chromospheric network without complementary data and the skill of an experienced observer. Analysis of imaging spectroscopy shows that line half-width and central intensity are correlated differently in coronal holes and a quiet Sun. This fact can be used to form linear combinations of these images in which coronal holes are better separated from the quiet Sun. Coronal hole borders agree well with SOHO/EIT data but can show significant differences from National Solar Observatory maps.


Spectroscopy Linear Combination Central Intensity Coronal Hole Imaging Spectroscopy 
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. Andretta, V., Jones, H. P.: 1997, Astrophys. J. 489, 375.CrossRefGoogle Scholar
  2. Avrett, E. N., Fontenla, J. M., and Loeser, R.: 1994, in D. M. Rabin, J. T. Jefferies, and C. Lindsey (eds.), Proceedings of the IAU Symposium on Infrared Solar Physics, Vol. 154, 35.Google Scholar
  3. Belkina, I. L., Akimov, L. A., Beletsky, S. A., Korokhin, V. V., andMarchenko, G. P.: 2000, Kinematika i Fizika Nebesnykh Tel 16, 316.Google Scholar
  4. Dupree, A. K., Penn, M. J., and Jones, H. P.: 1996, Astrophys. J., 467 L121.CrossRefGoogle Scholar
  5. Harvey, J. W., Krieger, A. S., Davis, J. M., Timothy, A. F., and Vaiana, G. S.: 1975, Bull. Amer. Astron. Soc. 7, 358.Google Scholar
  6. Harvey, K. L. and Recely, F.: 2002, Solar Phys. 211, 31.CrossRefGoogle Scholar
  7. Grammer, S. R., Kohl, J. L., and Noci, G.: 1999, Astrophys. J. 511, 481.CrossRefGoogle Scholar
  8. Jones, H. P.: 2003, Solar Phys. 218, 1.CrossRefGoogle Scholar
  9. Jones, H. P., Duvall, T. L. Jr., Harvey, J. W., Mahaffey, C. T., Schwitters, J. D., and Simmons, J. E.: 1992, Solar Phys. 139, 211.CrossRefGoogle Scholar
  10. Kahler, S. W., Davis, J. M., and Harvey, J. W.: 1983, Solar Phys. 87, 47.CrossRefGoogle Scholar
  11. Kulagin, E. S. and Kouprianov, V. V.: 2003, in Proceedings of the IAU Symposium on Multi-Wavelength Investogations of Solar Activity, Vol. 223 (abstract).Google Scholar
  12. Lemaire, P., Bocchialini, K., and Aletti, V.: 1999, Space Sci. Rev. 87, 249.CrossRefGoogle Scholar
  13. Malanushenko, O. V. and Jones, H. P.: 2002, Bull. Am. Astronom. Soc. 34, 700.Google Scholar
  14. Malanushenko, O. V. and Jones, H. P.: 2004, Solar Phys. 222, 43.CrossRefGoogle Scholar
  15. Malanushenko, V. P., Polosukhina, N. S., and Weiss, W. W.: 1992, Astron. Astrophys. 259, 567.Google Scholar
  16. Malanushenko E., Stepanian N. N., and Baranovsky E.: 2000, Workshop on Helium Line Formation in a Dynamical Solar Atmosphere, Naples, Italy, April 5–7 (talk).Google Scholar
  17. Malanushenko, E. V. and Stepanian, N. N.: 2001, Izv. Krymsk. Astrofiz. Observ. 97, 69 (in Russian).Google Scholar
  18. Stucki, K., Solanki, S. K., Schuhle, U., Ruedi, I., Wilhelm, K., Stenflo, J. O., Brkovic, A., and Huber, M. C. E. : 2000, Astron. Astrophys. 363, 1145.Google Scholar
  19. Venkatakrishnan, P., Jain, S. K., Singh, J., Recely, F., and Livingston, W. C.: 1992, Solar Phys. 138, 107.CrossRefGoogle Scholar
  20. Wilhelm, K., Marsch, E., Dwivedi, B. N., Hassler, D. M., Lemaire,P., Gabriel, A. H., and Huber, M. C. E.: 1998, Astrophys. J. 500, 1023.CrossRefGoogle Scholar
  21. Zirker, J. B. (ed.): 1977, Coronal Holes and High-Speed Wind Streams, Colorado Association University Press, Boulder.Google Scholar

Copyright information

© Springer Science + Business Media, Inc. 2005

Authors and Affiliations

  1. 1.National Solar ObservatoryTucsonU.S.A.
  2. 2.NASA’S GSFCU.S.A.

Personalised recommendations