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Phase Relations and Other Diagnostics of Solar Atmospheric Structure and Dynamics

Published online by Cambridge University Press:  08 February 2017

Franz - Ludwig Deubner
Franz - Ludwig Deubner*
Affiliation:
Astronomisches Institut der Universität Würzburg, D - 97074 Würzburg, Germany

Abstract

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Based on spectral observations with high spatial and temporal resolution, we discuss in this brief review the dynamic behaviour of the upper layers of the quiet solar atmosphere. A proper description of this behaviour is fundamental for the understanding (and simulation) of the temperature structure and the heating of the chromosphere, and the interpretation of such conspicuous phenomena like the chromospheric “grains”. The evidence is drawn from waveforms, power spectra, and phase spectra of velocity and brightness fluctuations in numerous Fraunhofer lines formed over an extended radial range of the atmosphere. A comparison with recent predictions of simulation calculations documents the strong need to extend the simulation codes to 3-D, and also to incorporate a realistic chromosphere/coronal transition layer, to better reproduce the observations.

Type
VII. The Solar Atmosphere
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 427 - 434
Copyright
Copyright © Kluwer 1998 

References

Bocchialini, K. and Koutchmy, S.: 1995, in Hoeksema, J.T., Domingo, V., Fleck, B., and Battrick, B. (eds.), Fourth SOHO Workshop: Helioseismology, ESA, p. 499.Google Scholar
Carlsson, M. and Stein, R.F.: 1993, in Maltby, P. and Pécsely, H.L. (eds.) Wave Phenomena in Solar Terrestrial Plasmas Univ. of Oslo, p. 21.Google Scholar
Carlsson, M. and Stein, R.F.: 1994, in Carlsson, M. (ed.), Chromospheric Dynamics, Univ. of Oslo, p. 47.Google Scholar
Carlsson, M. and Stein, R.F.: these proceedings .Google Scholar
Cheng, Q.Q. and Yi, Z.: 1996, Astron. Astrophys. 313, 971.Google Scholar
Deubner, F.-L.: 1976, Astron. Astrophys. 51, 189.Google Scholar
Deubner, F.-L.: 1990, in Stenflo, J.O. (ed.) Solar Photosphere: Structure, Convection, and Magnetic Fields IAU Symp. 138, 217.CrossRefGoogle Scholar
Deubner, F.-L.: 1991, in Ulmschneider, P., Priest, E.R., and Rosner, R. (eds.) Mechanisms of Chromospheric and Coronal Heating, Springer, p. 6.CrossRefGoogle Scholar
Deubner, F.-L.: 1995, in Ulrich, R. K., Rhodes, E. Jr., and Däppen, W. (eds.), Helio- and Asteroseismology from the Earth and Space, ASP Conf. Series 76, 303.Google Scholar
Deubner, F.-L., Endler, F., and Staiger, J.: 1984, Mem. S. A. Ital. 55, 135.Google Scholar
Deubner, F.-L., Waldschick, Th., and Steffens, S.: 1996, Astron. Astrophys. 307, 936.Google Scholar
Endler, F. and Deubner, F.-L.: 1983, Astron. Astrophys. 121, 291.Google Scholar
Fleck, B. and Deubner, F.-L.: 1989, Astron. Astrophys. 224, 245.Google Scholar
Fleck, B., Deubner, F.-L., Hofmann, J., and Steffens, S.: 1994, in Carlsson, M. (ed.), Chromospheric Dynamics, Univ. of Oslo, p. 103.Google Scholar
Gaizauskas, V.: 1985, in Lites, B. W. (ed.), Chromospheric Diagnostics and Modelling, Sunspot, N.M., p. 25.Google Scholar
Harvey, J.W., Duvall, T.L., Jefferies, S.M., Pomerantz, M.A.: 1993, in Brown, T.M. (ed.) GONG 1992: Seismic Investigation of the Sun and Stars, ASP Conf. Series 42, 111.Google Scholar
Hofmann, J., Steffens, S., and Deubner, F.-L.: 1996, Astron. Astrophys. 308, 192.Google Scholar
Jefferies, S.: these proceedings .Google Scholar
Jefferies, S., Osaki, Y., Shibahashi, H., Harvey, J.W., D'Silva, S., and Duvall, T.L. Jr.: 1997, Astrophys. J. 485, L 49.CrossRefGoogle Scholar
Lites, B.: 1994, in Carlsson, M. (ed.), Chromospheric Dynamics, Univ. of Oslo, p. 1.Google Scholar
Marmolino, C., Severino, G., Deubner, F.-L., and Fleck, B.: 1993, Astron. Astrophys. 278, 617.Google Scholar
Rutten, R.J.: 1995, in Hoeksema, J.T., Domingo, V., Fleck, B., and Battrick, B. (eds.) Fourth SOHO Workshop: Helioseismology, ESA, p. 151.Google Scholar
Rutten, R.J. and Uitenbroek, H.: 1991, Solar Phys. 134, 15.CrossRefGoogle Scholar
Severino, G.: 1997, private communication.Google Scholar
Skartlien, R., Carlsson, M., and Stein, R.F.: 1994, in Carlsson, M. (ed.), Chromospheric Dynamics, Univ. of Oslo, p. 79.Google Scholar
Staiger, J., Schmieder, B., Deubner, F.-L., and Mattig, W.: 1984, Mem. S. A. Ital. 55, 147.Google Scholar
Steffens, S., Deubner, F.-L., Fleck, B., and Wilhelm, K.: 1997a, in Wilson, A. (ed.), The Corona and Solar Wind Near Minimum Activity, ESA, p. 685.Google Scholar
Steffens, S., Deubner, F.-L., Fleck, B., Wilhelm, K., Harrison, R., and Gurman, J.: 1997b, in Wilson, A. (ed.), The Corona and Solar Wind Near Minimum Activity, ESA, p. 679.Google Scholar
Steffens, S., Deubner, F.-L., Hofmann, J., and Fleck, B.: 1995, Astro. Astrophys. 302, 277.Google Scholar
Steffens, S., Schmitz, F., and Deubner, F.-L.: 1997c, Solar Phys. 172, 85.CrossRefGoogle Scholar
Straus, Th., Deubner, F.-L., Fleck, B., Marmolino, C., Severino, G., and Tarbell, T.; these proceedings .Google Scholar
Worrall, G.: 1997, private communication.Google Scholar