[P-EM11] Frontiers in solar physics

[PEM11-02] The heating of the Sun’s Outer Atmosphere: Insights from Modeling and Observations

★Invited Papers

*Mah Asgari-Targhi¹、Shinsuke Imada² (1.Harvard-Smithsonian Center for Astrophysics, USA、2.Department of Earth and Planetary Science, University of Tokyo, Japan)

キーワード：Coronal Heating , Non-thermal Velocity, Magnetohydrodynamic (MHD) Waves, Chromospheric Heating

The solar corona is heated by the dissipation of magnetic disturbances that originate from the Sun’s convective motions. These convective flows interact with photospheric magnetic flux, generating magnetohydrodynamic (MHD) waves that propagate along flux tubes and dissipate their energy in the corona. In this presentation, I will discuss results from a 3D MHD model that explores the propagation and dissipation of Alfvén waves within coronal loops. The heating of the chromosphere may also be linked to this turbulence, with wave energy partially transmitted through the transition region, generating coronal turbulence. Our findings suggest that the hot (~3 MK) coronal loops commonly observed in active regions can be explained by Alfvén wave turbulence. We examine how these turbulence-driven heating mechanisms manifest in observational data, comparing spectral line widths measured by current instruments with expectations for future missions like Solar-C. These results support the idea that both coronal loops and the underlying chromosphere are heated by Alfvénic turbulence.