Primary Convener:
Rohit Chhiber, University of Delaware

Convener:
Mahboubeh Asgari-Targhi, Harvard-Smithsonian Center for Astrophysics
Federico Fraschetti, Harvard-Smithsonian Center for Astrophysics
Chingam Fong, Chinese University of Hong Kong

Early Career Convener:
Rahul Sharma, Northumbria University

Chair:
Rohit Chhiber, University of Delaware
Federico Fraschetti, Harvard-Smithsonian Center for Astrophysics
William Matthaeus, University of Delaware
Takeru Suzuki, Tokyo University

Magnetohydrodynamic turbulence is increasingly recognized as a key process driving coronal heating, solar wind acceleration, and energetic-particle transport. In-situ measurements have provided crucial insights into turbulent processes in the high corona and interplanetary medium, leaving the origin and injection of turbulence in the lower solar atmosphere poorly understood. The transition of turbulence across different regimes—from the partially-ionized photosphere/chromosphere to the fully-ionized corona—remains a crucial, yet largely unquantified component of overall energy transport and dissipation. Recent advances in high-resolution space-borne (e.g., SDO, IRIS, Hinode, SolO) and ground-based (e.g., SST, BBSO, DKIST) instrumentation offer a unique window to investigate these processes and provide important constraints for models. This session invites contributions addressing the onset and evolution of turbulence between the photosphere and lower solar atmosphere, its observable signatures, and implications for coronal and solar wind models and cosmic ray transport in the heliosphere. We welcome abstracts from both observational and theoretical perspectives.

Index Terms
7509 Corona
7514 Energetic particles
7529 Photosphere
7863 Turbulence

Cross-Listed:
NG - Nonlinear Geophysics
SM - SPA-Magnetospheric Physics

Neighborhoods:
4. Beyond Earth

Suggested Itineraries:
Space Weather