Energy Input Flux in the Quiescent Solar Corona: Comparing Observations with the AWSOM Model

NUEVO, FEDERICO A.; VAN DER HOLST, BARTHOLOMEUS; MAC CORMACK, CECILIA; VÁSQUEZ, ALBERTO M.; LANDI, ENRICO; LLOVERAS, DIEGO G.; MANCHESTER, WARD IV; FRAZIN, RICHARD A.

Ciudad de Buenos Aires

Conferencia; COLAGE XI; 2018

ALAGE

To remain stable, the million-Kelvin solar corona structures require a coronal heating rate efficient enough to compensate the radiative losses and the heat conductive flux. The energy provided by the (yet uncertain) coronal heating mechanism is ultimately injected at the coronal base. The energy input flux required at the coronal base can be estimated by means of differential emission measure tomography (DEMT) of EUV images, which allows studying the inner quiescent corona at a global scale. In this work we compare the energy-related tomographic results with those derived from magnetohydrodynamic three-dimensional (3D) simulations of the corona by means of the Alfvén Wave Solar Model (AWSOM). We present here first results of such validation effort.