Abstract
The fractional convective flux πF c (x c /πF) is computed for the effective level x c = logτ c = 0.125, using bi-dimensional co-spectra for relative continuum-brightness fluctuations ΔI and radial velocity fluctuations ΔV measured for the C i 5052.16 spectral line. A more uncertain flux for x Fe ≈ - 0.9 is obtained for the Fe i 5049.83 line. Since the results (Figure 1) incorporate current uncertainties in RMS ΔI , RMS ΔV and RMS ΔT (x), where ΔT are photospheric temperature fluctuations, they must be considered qualitative until these uncertainties are appreciably reduced. The requirement that the fractional convective flux < 1, places restrictions on these uncertainties which suggest that current RMS ΔT (x)'s are too large.
The results confirm the importance of overshoot at the top of the solar hydrogen convection zone and suggest a non-negligible fractional convective flux throughout the lower photosphere. Qualitatively, they do not agree with the predictions of the generally-used, local, mixing-length theory or those of Parsons' (1969) modified mixing-length theory. However, qualitative agreement with the predictions of the non-local, generalized mixing-length theory of Spiegel (1963) and with the non-local theory of Ulrich (1970) cannot be considered as observational confirmation of these theories.
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References
Bahng, J. and Schwarzschild, M.: 1961, Astrophys. J. 134, 337.
Carbon, D. F. and Gingerich, O.: 1969 in Gingerich, O. (ed.), Theory and Observation of Normal Stellar Atmospheres, Proc. 3rd Harvard-Smithsonian Conf. on Stellar Atmospheres (MIT Press), p. 377.
De Jager, C.: 1972, Solar Phys. 25, 71.
Edmonds, F. N., Jr.: 1962, Astrophys. J. Suppl. 6, 357.
Edmonds, F. N., Jr.: 1964, Astrophys. J. 139, 1358.
Edmonds, F. N., Jr. and Hinkle, K. H.: 1974, in preparation.
Edmonds, F. N., Jr. and Webb, C. J.: 1972, Solar Phys. 25, 44.
Edmonds, F. N., Jr., Michard, R., and Servajean, R.: 1965, Ann. Astrophys. 28, 534.
Gingerich, O., Noyes, R. W., Kalkofen, W., and Cuny, Y.: 1970, Solar Phys. 18, 347.
Heintze, J. R. W., Hubenet, H., and De Jager, C.: 1964, Bull. Astron. Inst. Neth. 17, 442.
Hinkle, K. H.: 1974, in preparation.
Ledoux, P., Schwarzschild, M., and Spiegel, E. A.: 1961, Astrophys. J. 133, 184.
Leighton, R. B.: 1963, Ann. Rev. Astron. Astrophys. 1, 19.
Michelis, C.-H.: 1974, private communication.
Mullan, D. J.: 1971, Monthly Notices Roy. Astron. Soc. 154, 467.
Nordlund, Å.: 1974, Astron. Astrophys. 32, 407.
Parsons, S. B.: 1969, Astrophys. J. Suppl. 18, 127.
Reiling, H.: 1971, Solar Phys. 19, 297.
Ross, J. E.: 1973, Joint meeting of Commissions 14, 29, and 45, 15th General Assembly of the IAU, Sydney, Aug. 21–30.
Spiegel, E. A.: 1963, Astrophys. J. 138, 216.
Travis, L. D. and Matsushima, S.: 1973, Astrophys. J. 180, 975.
Ulrich, R. K.: 1970, Astrophys. Space Sci. 7, 183.
Unno, W.: 1969, Publ. Astron. Soc. Japan 21, 240.
Wilson, P. R.: 1969, Solar Phys. 9, 303.
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Edmonds, F.N. Convective flux in the solar photosphere as determined from fluctuations. Sol Phys 38, 33–41 (1974). https://doi.org/10.1007/BF00161821
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DOI: https://doi.org/10.1007/BF00161821