Abstract
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.
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References
Andretta, V., Jones, H. P.: 1997, Astrophys. J. 489, 375.
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.
Belkina, I. L., Akimov, L. A., Beletsky, S. A., Korokhin, V. V., andMarchenko, G. P.: 2000, Kinematika i Fizika Nebesnykh Tel 16, 316.
Dupree, A. K., Penn, M. J., and Jones, H. P.: 1996, Astrophys. J., 467 L121.
Harvey, J. W., Krieger, A. S., Davis, J. M., Timothy, A. F., and Vaiana, G. S.: 1975, Bull. Amer. Astron. Soc. 7, 358.
Harvey, K. L. and Recely, F.: 2002, Solar Phys. 211, 31.
Grammer, S. R., Kohl, J. L., and Noci, G.: 1999, Astrophys. J. 511, 481.
Jones, H. P.: 2003, Solar Phys. 218, 1.
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.
Kahler, S. W., Davis, J. M., and Harvey, J. W.: 1983, Solar Phys. 87, 47.
Kulagin, E. S. and Kouprianov, V. V.: 2003, in Proceedings of the IAU Symposium on Multi-Wavelength Investogations of Solar Activity, Vol. 223 (abstract).
Lemaire, P., Bocchialini, K., and Aletti, V.: 1999, Space Sci. Rev. 87, 249.
Malanushenko, O. V. and Jones, H. P.: 2002, Bull. Am. Astronom. Soc. 34, 700.
Malanushenko, O. V. and Jones, H. P.: 2004, Solar Phys. 222, 43.
Malanushenko, V. P., Polosukhina, N. S., and Weiss, W. W.: 1992, Astron. Astrophys. 259, 567.
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).
Malanushenko, E. V. and Stepanian, N. N.: 2001, Izv. Krymsk. Astrofiz. Observ. 97, 69 (in Russian).
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.
Venkatakrishnan, P., Jain, S. K., Singh, J., Recely, F., and Livingston, W. C.: 1992, Solar Phys. 138, 107.
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.
Zirker, J. B. (ed.): 1977, Coronal Holes and High-Speed Wind Streams, Colorado Association University Press, Boulder.
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Malanushenko, O.V., Jones, H.P. Differentiating Coronal Holes from the Quiet Sun by He 1083 nm Imaging Spectroscopy. Sol Phys 226, 3–16 (2005). https://doi.org/10.1007/s11207-005-4972-z
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DOI: https://doi.org/10.1007/s11207-005-4972-z