Abstract
We examine the progress made during the last decade in our knowledge of stellar convection, first in the theory and using numerical simulation, and second through observations, from ground and space.
Special emphasis is put on those results which allow to tackle the basic questions: i. Is the same mechanism responsible for the different types and scales of motions that are currently identified in the solar convection zone: granulation, mesogranulation, supergranulation, large eddies? ii. On which scale(s) is energy injected into the convective motions? For what reason?
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Zahn, J.P. (1987). Solar and stellar convection. In: Schröter, EH., Schüssler, M. (eds) Solar and Stellar Physics. Lecture Notes in Physics, vol 292. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0032311
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DOI: https://doi.org/10.1007/BFb0032311
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