Abstract
We discuss a theoretical method of computing the temperature structure of hot and cool streams in convective stellar atmospheres. The method is based on the model that the streams are due to organized cells whose diameters are greater than the thickness of the photosphere. The excess thermal energy of matter rising from the deeper layers, where the entropy is higher than in the photosphere, is converted to radiation in a steady front. This model, applied to the solar case, exhibits a peak-to-peak contrast of 30–40% between granules and lanes. This contrast agrees with the Stratoscope data reduced by Namba and Diemel (1969). As a necessary part of the theory, we obtain an expression for the perturbation in radiative heat exchange which may be used in a medium with a strongly preferred direction such as a stellar atmosphere.
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References
Bahng, J. and Schwarzschild, M.: 1961a,Astrophys. J.,134, 312.
Bahng, J. and Schwarzschild, M.: 1961b,Astrophys. J. 134, 337.
Banos, G.: 1968,Ann. Astrophys. 31, 501.
Böhm, K. H.: 1954,Z. Astrophys. 35, 179.
Böhm-Vitense, E.: 1958,Z. Astrophys. 46, 108.
de Jager, C.: 1959,Handbuch der Physik (ed. by. S. Flügge) Springer-Verlag, Berlin,52, 80.
de Jager, C. and Neven, L.: 1968,Solar Phys. 1, 27.
de Jager, C. and Neven, L.: 1968,Solar Phys. 4, 379.
Demarque, P. B. and Percy, J. R.: 1964,Astrophys. J. 140, 541.
Edmonds, F. N.: 1962,Astrophys. J. Suppl 6, 357.
Elste, G. E.: 1967,Astrophys. J. 148, 859.
Gingerich, O. and de Jager, C.: 1968,Solar Phys. 3, 5.
Kourganoff, V.: 1963,Basic Methods in Transfer Problems, Dover, New York, p. 45.
Lambert, D. L. and Mallia, E. A.: 1968,Solar Phys. 3, 499.
Leighton, R. B.: 1963,Ann. Rev. Astron. Astrophys. 1, 19.
Margrave, T. E. and Swihart, T. L.: 1969,Solar Phys. 5, 12.
Morton, B. R., Taylor, G. I., and Turner, J. S.: 1956,Proc. Roy. Astron. Soc. London 234A, 1.
Namba, O. and Diemel, W. E.: 1969,Solar Phys. 7, 167.
Rosche, J.: 1959,Ann. Astrophys. 22, 584.
Spiegel, E. A.: 1957,Astrophys. J. 126, 202.
Swihart, T. L.: 1966,Astrophys. J. 143, 358.
Torres-Peimbert, S., Simpson, E., and Ulrich, R. K.: 1969,Astrophys. J. 156, 559.
Turner, J. S.: 1964,J. Fluid. Mech. 19, 481.
Ulrich, R. K.: 1970a,Astrophys. Space Sci. 7, 71.
Ulrich, R. K.: 1970b,Astrophys. Space Sci. 7, 183.
Unno, W.: 1959,Astrophys. J. 129 375.
Unno, W.: 1965,Publ. Astron. Soc. Japan 17, 205.
Unno, W. and Spiegel, E. A.: 1966,Publ. Astron. Soc. Japan 18, 85.
Wilson, P. R.: 1968,Astrophys. J. 142, 1195.
Wilson, P. R.: 1969,Solar Phys. 6, 364.
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Supported in part by the National Science Foundation [GP-15911 (formerly GP-9433), GP-9114] and the Office of Naval Research [Nonr-220(47)].
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Ulrich, R.K. Convective energy transport in stellar atmospheres. Astrophys Space Sci 9, 80–96 (1970). https://doi.org/10.1007/BF00649954
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DOI: https://doi.org/10.1007/BF00649954