The solar temperature reversal and convective motions

Abstract

Given an equation of State, the three equations of mass, momentum and energy conservation determine the vortex free flow fields in a star. The solar data processed by Athay (1966) is a measure of the dissipation of the fluid, while the use of an empirical temperature profile (BCA, 1968) permits values for the gradients in the equations of fluid flow rendering them algebraic, with solutions independent of boundary conditions. This approach serves as a consistency check on the methods with which data have been processed by inquiring to what degree the basic conservation laws have been satified, and by directly implying a velocity field which can be scrutinized for its observational consequences.

We find that the most consistent interpretation to this data is that the temperature minimum should not be coincident with flux maximum as the BCD model photosphere is, and that the temperature profile must rise higher at the 1500 km. region above optical depth one. Furthermore, more emissions must occur in the U-V metals at this region to support such a temperature increase, but at least an order of magnitude decrease in H⁻ emission should also be expected, as well as some suppression of the Balmer. As a theoretical consequence horizontal stratification of the velocity field occurs, suggesting either cellular motions or differential rotation with surface velocities as high as 60 km s⁻¹, but on the average near 30 to 40 km s⁻¹, across the solar surface.