Abstract
The radio brightness distribution at λ9 mm, λ3.5 mm and λ1.2 mm is calculated employing a statistical technique to account for the presence of spicules randomly occurring along the ray path. The results indicate limb brightening at each wavelength when the Avery and House (1969) spicule model is employed. This contradicts the results of Lantos and Kundu (1972) whose method of computation is shown to be inadequate.
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References
Ade, P. A. R., Rather, J. D. G., and Clegg, P. E.: 1974, Astrophys. J. 187, 389.
Avery, L. W. and House, L. L.: 1969, Solar Phys. 10, 88.
Beckers, J. M.: 1968, Solar Phys. 3, 367.
Beckers, J. M.: 1972, Ann. Rev. Astron. Astrophys. 10, 73.
Cuny, Y.: 1971, Solar Phys. 16, 293.
Dupree, A. K. and Goldberg, L.: 1967, Solar Phys. 1, 229.
Lantos, P.: 1972, Solar Phys. 22, 2.
Lantos, P. and Kundu, M. R.: 1972, Astron. Astrophys. 21, 119.
Vernazza, J. E., Avrett, E., and Loeser, R.: 1973, Astrophys J. 181, 605.
Withbroe, G. L.: 1970, Solar Phys. 11, 208.
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Kalaghan, P.M. Solar limb brightening at millimeter wavelengths. Sol Phys 39, 315–322 (1974). https://doi.org/10.1007/BF00162424
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DOI: https://doi.org/10.1007/BF00162424