Understanding magnetically-driven processes in the quiet Sun is crucial for understanding chromospheric and coronal heating. The main goal of our study is to quantify the energy output of the quiet Sun photosphere. The amount of magnetic energy being transported upwards from the photosphere can be expressed in terms of the vertical component of Poynting flux, which is a cross-product of magnetic and electric fields. While magnetic fields and energy fluxes within active regions and plage have been evaluated before, quiet Sun magnetograms have only recently become available with the launch of missions such as Hinode and Sunrise and the Daniel K. Inouye Solar Telescope (DKIST) coming online early this year. In this presentation, we present estimates of Poynting flux using IMaX data. As the electric field E is one of the two principal quantities required to compute Poynting flux, we use two distinct approaches to infer E. In the first approach, we derive the electric field using ideal plasma assumption with horizontal velocities obtained from the convolutional neural network (DeepVel, Asensio Ramos et al. 2017). In the second approach, we derive E using the PDFI-SS approach uncurling Faraday's law (Fisher et al. 2020). We discuss the distribution of Poynting flux and whether it is sufficient to explain chromospheric and coronal heating.
44th COSPAR Scientific Assembly. Held 16-24 July
- Pub Date:
- July 2022