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Theoretical Understanding of Chromospheric Inhomogeneities

Published online by Cambridge University Press:  06 September 2019

Philippe Delache
Philippe Delache*
Affiliation:
Observatoire de Nice

Extract

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“By assuming that the atmosphere is

homogeneous at each depth, we are

immeasurably adding to the numerical

tractability of the problem at the

expense of ignoring 80 years' worth

of data on chromospheric inhomogeneities”

Linsky and Avrett (1970)

To the spatial inhomogeneity, Linsky and Avrett could have added the variations with time which are also well known, well observed characteristics of the solar chromosphere. Let me quote also Praderie (1969): large asymmetries are observed in stellar K2 components which vary with time, “so that it seems difficult to think of any interpretation of the K line profile that would ignore motions and inhomogeneities in the atmosphere of those stars” And let me borrow a conclusion from Thomas (1969): “So what we need are ingenious ideas for empirical inference; or theoretical generalization from experience with the solar case” I wonder if the solar experience is sufficient at the present time to permit any theoretical generalization, as has been the case for the solar wind. In order to simplify, I shall restrict the scope of this contribution to the quiet solar chromosphere, and focus only on spicules.

Type
Part III: Mechanical heating and its Effect on the Chromospheric Energy Balance
Information
International Astronomical Union Colloquium , Volume 19: Stellar Chromospheres , February 1973 , pp. 207 - 218
Copyright
Copyright © Nasa 1972

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