Abstract
Existing models of the quiet chromosphere-corona transition region predict a distribution of emission measure over temperature that agrees with observation for T ≳ 105 K. These ‘network’ models assume that all magnetic field lines that emerge from the photosphere extend into and are in thermal contact with the corona. We show that the observed fine-scale structure of the photospheric magnetic network instead suggests a two-component picture in which magnetic funnels that open into the corona emerge from only a fraction of the network. The gas that makes up the hotter transition region is mostly contained within these funnels, as in standard models, but, because the funnels are more constricted in our picture, the heat flowing into the cooler transition region from the corona is reduced by up to an order of magnitude. The remainder of the network is occupied by a population of low-lying loops with lengths ≲ 104 km. We propose that the cooler transition region is mainly located within such loops, which are magnetically insulated from the corona and must, therefore, be heated internally. The fine-scale structure of ultraviolet spectroheliograms is consistent with this proposal, and theoretical models of internally heated loops can explain the behavior of the emission measure below T ≈ 105 K.
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Antiochos, S. K. and Noci, G.: 1985, ‘The Structure of the Static Corona and Transition Region’, Preprint No. CSSA-ASTRO-85-13.
Athay, R. G.: 1981a, Astrophys. J. 249, 340.
Athay, R. G.: 1981b, in S. Jordan (ed.), The Sun as a Star, NASA SP-450, p. 85.
Athay, R. G.: 1982, Astrophys. J. 263, 982.
Bonnet, R. M., Bruner, E. C., Jr., Acton, L. W., Brown, W. A., and Decaudin, M.: 1980, Astrophys. J. 237, L47.
Dere, K. P., Bartoe, J.-D. F., and Brueckner, G. E.: 1983, Astrophys. J. 267, L65.
Dere, K. P., Bartoe, J.-D. F., and Brueckner, G. E.: 1984, Astrophys. J. 281, 870.
Doschek, G. A., Feldman, U., and Bohlin, J. D.: 1976, Astrophys. J. 205, L177.
Dowdy, J. F., Moore, R. L., and Wu, S. T.: 1985, Solar Phys. 99, 79.
Feldman, U.: 1983, Astrophys. J. 275, 367.
Feldman, U., Doschek, G. A., and Mariska, J. T.: 1979, Astrophys. J. 229, 369.
Gabriel, A. H.: 1976, Phil. Trans. Roy. Soc. London A281, 339.
Giovanelli, R. G.: 1982, Solar Phys. 77, 27.
Harvey, J.: 1976, in E. A. Muller (ed.), IAU Highlights of Astronomy, Vol. 4, Part II.
Howard, R. and LaBonte, B. J.: 1981, Solar Phys. 74, 131.
Huber, M. C. E., Foukal, P. V., Noyes, R. W., Reeves, E. M., Schmahl, E. J., Timothy, J. G., Vernazza, J. E., and Withbroe, G. L.: 1974, Astrophys. J. 194, L115.
Livingston, W. C. and Harvey, J.: 1975, Bull. Am. Astron. Soc. 7, 346.
Rabin, D. and Moore, R.: 1984, Astrophys. J. 285, 359.
Reeves, E. M.: 1976, Solar Phys. 46, 53.
Reeves, E. M., Vernazza, J. E., and Withbroe, G. L.: 1976, Phil. Trans. Roy. Soc. London A281, 319.
Sheeley, N. R., Jr.: 1981, in F. Q. Orrall (ed.), Solar Active Regions, Colorado Associated University Press, Boulder, p. 17.
Withbroe, G. L.: 1983, Astrophys. J. 267, 825.
Withbroe, G. L. and Noyes, R. W.: 1977, Ann. Rev. Astron. Astrophys. 15, 363.
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Dowdy, J.F., Rabin, D. & Moore, R.L. On the magnetic structure of the quiet transition region. Sol Phys 105, 35–45 (1986). https://doi.org/10.1007/BF00156374
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DOI: https://doi.org/10.1007/BF00156374