Temporal Relation between Disappearance of Penumbral Fine-Scale   Structure and Evershed Flow
  We investigate the temporal relation between the Evershed flow, dot-like bright features (penumbral grain), the complex magnetic field structure, and dark lanes (dark core) along bright filaments in a sunspot penumbra. We use a time series of high spatial resolution photospheric intensity, vector magnetic field maps, and Doppler velocity maps obtained with the Solar Optical Telescope aboard the \textit{Hinode} spacecraft. We conclude that the appearance and disappearance of the Evershed flow and penumbra grains occur at nearly the same time and are associated with changes of the inclination angle of the magnetic field from vertical to more horizontal. This supports the idea that Evershed flow is a result of thermal convection in the inclined field lines. The dark core of the bright penumbral filament also appears coincidental with the Evershed flow. However, the dark-cored bright filament survives at least for 10-20 minutes after the disappearance of the Evershed flow. The heat input into the bright filament continues after the end of heat transfer by the Evershed flow. This suggests that local heating along the bright filament is important to maintain the brightness of the bright filament in addition to the heat transfer by the Evershed flow. 
M. Kubo, K. Ichimoto, B. W. Lites, and R. A. Shine
astro-ph.SR