Abstract
Study of the generation and propagation of waves in the solar convection zone and atmosphere began with the realization in the late 1940s that such waves could carry mechanical energy from the turbulent convection zone into the chromosphere and corona. Dissipation of these waves could then produce the observed increase in temperature in the outer atmosphere of the Sun, and could explain much, if not all, of the observed nonthermal broadening of solar spectrum lines. Such propagating waves are difficult to observe, largely because they are transient and of small spatial scale, and one is often reduced to inferring their presence from a combination of indirect observations together with a chain of theoretical arguments. Further difficulties arise in both theory and observation because the waves become highly nonlinear in the chromosphere and corona and experience strong nonadiabatic effects in and just below the photosphere. These effects are extremely difficult to model accurately, hence the waveforms are largely unknown.
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Brown, T.M., Mihalas, B.W., Rhodes, E.J. (1986). Solar Waves and Oscillations. In: Sturrock, P.A., Holzer, T.E., Mihalas, D.M., Ulrich, R.K. (eds) Physics of the Sun. Geophysics and Astrophysics Monographs, vol 24. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5253-9_7
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DOI: https://doi.org/10.1007/978-94-009-5253-9_7
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8819-0
Online ISBN: 978-94-009-5253-9
eBook Packages: Springer Book Archive