Abstract
Observations of the quiet sun at wavelengths from 3 Å to 75 cm show (with two exceptions: the Ovi line at 1032 Å and possibly the continuum at 1.2 mm) either no limb brightening or less than had been supposed. On the other hand, the brightness temperature is observed to increase with wavelength in the millimeter and centimeter range. If this increase is due to greater visibility of hot overlying material, that material ought to be evident at the limb at shorter wavelengths, resulting in limb brightening. The only possible explanation for the absence of limb brightening at almost all wavelengths is that the emitting surface is rough at all wavelengths, with a scale of roughness approximately equal to the scale height at each temperature. Contradictions with existing models, along with the additional observations required for an improved model are discussed.
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References
Allen, C. W.: 1963,Astrophysical Quantities, Oxford University Press, New York.
Alon, I., Arsac, J., and Steinberg, J. L.: 1953,Compt. Rend. 237, 300.
Athay, R. G.: 1959, Paris Symposium on Radio Astronomy.
Bonnett, R. M. and Blamont, J. E.: 1968,Solar Phys. 3, 64.
Buhl, D. and Tlamicha, A.: 1968,Astrophys. J. Letters 153, L189.
Coates, R. J.: 1958,Astrophys. J. 128, 83.
Coates, R. J., Gibson, J. E., and Hagen, J. P.: 1958,Astrophys. J. 128, 406.
Gingerich, O. and De Jager, C.: 1968,Solar Phys. 3, 5.
Kundu, M.: 1965,Solar Radio Astronomy, Interscience, New York.
Lena, P. J.: 1968,Solar Phys. 3, 28.
Little, A. G.: 1967,Proc. A.S.A. 1, 42.
Moffet, A. T.: 1967, personal communication.
Moriyama, F.: 1961,Ann. Tokyo Astron. Obs. 7, 132.
Newkirk, G.: 1961,Astrophys. J. 133, 982.
Newstead, R.: 1969,Solar Phys. (in press).
Noyes, R. W. and Goldberg, L.: 1968, AAS Special Solar Mtg., Tucson, Ariz.
Noyes, R. W., Beckers, J. M., and Low, F. J.: 1968,Solar Phys. 3, 36.
Riddle, A. C.: 1969,Solar Phys. (in press).
Shimabukuro, F. I.: 1969, preprint.
Shimabukuro, F. I. and Stacey, J. M.: 1968,Astrophys. J. 152, 777.
Simon, M.: 1965,Astrophys. J. 141, 1513.
Swarup, G.: 1961, Rept. No. 13, Stanford Electronics Laboratories, Stanford, Calif.
Tlamicha, A.: 1968, personal communication.
Tousey, R.: 1967,Astrophys. J. 149, 239.
Vaiana, G. S., Reidy, W. P., Zehnpfennig, T., Van Speybroeck, L., Giaconni, R.: 1968,Science 161, 564.
Van de Hulst, H. C.: 1950,Bull. Astron. Inst. Netherlands 11, 135.
Zirin, H. and Dietz, R. D.: 1963,Astrophys. J. 138, 664.
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This research was supported by the National Science Foundation under GP-7030 and the National Aeronautics and Space Administration under grant NGR 05 002 034.
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Simon, M., Zirin, H. The coarse structure of the solar atmosphere. Sol Phys 9, 317–327 (1969). https://doi.org/10.1007/BF02391654
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DOI: https://doi.org/10.1007/BF02391654