The Importance of Horizontal Poynting Flux in the Solar Photosphere

Abstract The electromagnetic energy flux in the lower atmosphere of Sun is a key tool to describe balance solar atmosphere. Current investigations on focus primarily vertical through photosphere, ignoring Poynting other directions and its possible contributions local heating. Based realistic Bifrost simulation quiet-Sun (coronal hole) atmosphere, we find that total photosphere occurs mainly parallel concentrating small regions along intergranular lanes. Thereby, it was define proxy for this based only variables can be promptly retrieved from observations, namely, horizontal velocities small-scale magnetic elements their longitudinal flux. Our accurately describes actual distribution simulations, with reaching 10 erg cm −2 s −1 . To validate our findings, extended analysis Sunrise /IMaX data. First, show realistically photospheric regions, as presents similar distributions line-of-sight velocity field. Second, found very simulated observational results also indicate observations considerably larger than previous estimates. Therefore, confirms most intense localized