Flow speed inside the brightness boundary of coronal streamers

Abstract

Density measurements in the legs of coronal streamers, where there might be outflow, are reproduced here using a magnetohydrodynamic model of the flow inside the brightness boundary of streamers. The model returns values for the flow speed and stream tube geometry (spreading) between the base and a few solar radii. The flow speed is consistent with there being no measurable outflow below 2.5 R_$\odot$ and an outflow of ~100 km/s at 5 R_$\odot$. We briefly describe the model, observations, and physical interpretation.