Dynamical model of convection in stellar cores
Yin-Ching Lo and
Received 6 March 1996 / Accepted 2 December 1996
In this work, the classical mixing-length theory is left aside and an alternative picture of convection is considered. This new model assumes that, in stellar conditions, convective transport is mainly achieved by turbulent plumes. This means of energy transport has been examined recently in the context of convective envelopes. Herein, the same approach is applied to the case of convective cores where the physical conditions are somewhat different. We show that turbulent plumes can indeed exist in such domains and may be efficient in the transport of heat. Unfortunately, a free parameter is introduced: the model does not constrain the total number of plumes. However, limits on the value of this parameter are given and the results obtained within these limits do not vary too drastically. Overshooting from convective cores is further evidenced in this model.
Key words: convection waves stars: interior
Send offprint requests to: Y.-C. Lo (email@example.com)
© European Southern Observatory (ESO) 1997
Online publication: June 5, 1998