Abstract:

By simulating the convection in the upper layers of six different stars and matching these simulations to 1D-mixing length models using the same input physics, we have been able to infer the behaviour of the mixing-length parameter, , as the stellar parameters changes.

solar physics, convection, hydrodynamics

• Introduction
• The selected stars
• The convection simulations
• The envelope models
• Matching envelope-models to the simulations
• Conclusions
• References
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