A Simplified Transport Model for sub-Alfvénic Flows in the Corona

Modeling the solar "wind" in the corona presents a different set of challenges than in parts further out in the heliosphere. Within the corona, the flows are sub-Alfvénic (V_A ≫ U), with the gradients of the Alfvén speed leading to generation of inward and outward fluctuations. Further challenges come from the (likely) lack of a strong turbulent cascade and the high temperatures ( ∼ Million Kelvin) within the corona. We present work to model sub-Alfvénic flows in the corona. We focus on a more simplified approach to the model by examining the transport of fluctuation energies, their associated length scale, and temperatures. We discuss each of the issues above and how they affect the model. The Alfvén speed profile is specified based on other simulations, the possible lack of a strong turbulent cascade leads to different models for the non-linear terms, and the temperature derives from the dissipation caused by the non-linear terms. All these issues will be discussed and incorporated into the model. Overall, the model emphasizes relatively basic physics but provides promising beginning results.