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Published online by Cambridge University Press:  30 March 2016

D. J. Mullan
D. J. Mullan*
Affiliation:
Bartol Research Foundation of the Franklin Institute Swarthmore, Pennsylvania, USA

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Heterogeneities in the solar atmosphere exist on many different length scales ranging from values as large as the solar radius (~106 km) down to features which are identifiable only by interferometry (~102 km). Rather than simply cataloguing the observed parameters of each and every known type of heterogeneity, I would like to concentrate on a few types of heterogeneities, with a view to identifying the information which is currently available concerning the physical mechanisms responsible for creating the in homogeneities. It is only if we can first identify the physics of each type of heterogeneity that we can hope to take even the first step towards predicting how each particular heterogeneity should scale to other stars. Since the present session is a joint discussion among mainly stellar astronomers, I feel that this approach is probably the most favorable method to present some of the large amount of information now available on solar features. Of course we expect that our solar information will be of most use to stellar astronomers in interpreting observations of stars which have similar spectral types to the sun. Nevertheless, we hope that nature will be kind enough to allow us to scale at least some of our information over a non-negligible area in the H.R. diagram.

Type
Joint Meeting
Information
Highlights of Astronomy , Volume 4 , Issue 2: Highlights of Astronomy. As presented at the XVIth General Assembly of the IAU, 1976 (Part II) , 1977 , pp. 375 - 387
Copyright
Copyright © Reidel 1977

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