Abstract
An equatorial coronal hole has been observed on 18 and 19 October 1996 with SOHO-CDS and with the Nancąy Radioheliograph (RH). The CDS EUV line intensities are used to determine the coronal hole Differential Emission Measure (DEM); in turn this is used to compute the radio brightness temperature Tb at the observed frequencies, leaving the coronal electron temperature and density as free parameters. EUV line intensities, calculated from the derived models, show a good agreement with EUV observations.
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References
Chiuderi Drago, F.: 1980, Solar Phys., 65, 237.
David, C., Gabriel, A. H., Bely-Dubau, F., Fludra, A., Lemaire, P., and Wilhelm, K.: 1998, A&A, 336, L90.
Fludra, A., Del Zanna, G., Alexander, D., and Bromage, B.: 1998, J. Geophys. Res., in press.
Hara, H., Tsuneta, S., Acton, L. W., and Ogawara, Y.: 1994, Pub. Astr. Soc. Jap., 46, 493.
Kerdraon, A., and Delouis, J. M.: 1997, in Coronal Physics from Radio and Space Observations, ed. G. Trottet, 483, 192.
Landi, E., and Landini, M.: 1997, A&A, 327, 1230.
Landi, E., and Landini, M.: 1998, A&A, in press.
Landi, E., Landini, M., Dere, K., Young, P., and Mason, H.: 1999, A&ASS, in press.
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Chiuderi-Drago, F., Kerdraon, A., Landi, E. et al. EUV and Radio Observations of an Equatorial Coronal Hole. Space Science Reviews 87, 141–144 (1999). https://doi.org/10.1023/A:1005138804659
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DOI: https://doi.org/10.1023/A:1005138804659