Chromospheric and TR diagnostics in a large scale numerical simulation of flux emergence: Synthetic vs Real observables

Abstract:

Field stored just below or rising to the photosphere will break through the surface and enter the upper atmosphere once the gradient of the subphotospheric field strength becomes sufficiently large. Opposite polarity flux bundles will reconnect in the photosphere and above, to form steadily longer loops that expand into the outer solar atmosphere, forming the corona. Some of the emerging flux is likely due to a local dynamo, but also the direct emergence of large scale magnetic structures from below is important, even in the quiet Sun. A significant proportion of this field likely reaches the chromosphere and may leave imprint on chromospheric dynamics and energetics. Using large scale numerical models (72x72x60) Mm and the high resolution spectra and slit jaw images from IRIS, as well as photospheric data from Hinode/SOT, and SDO/HMI we study the interactions between the magnetic flux caught in the granular flow field and the chromosphere and chromospheric field above. We will compare synthetic observables of the photospheric Fe I 617.3 nm line, the chromospheric Mg II h&k lines, and the transition region Si IV lines, with their observational counterparts. We will also generate synthetic ALMA band 3 images. The comparison of synthetic observational data will let us draw conclusions as to the validity of the numerical modeling and the importance of flux emergence for the dynamics and energetics of the outer solar atmosphere.