Magnetic waves are considered one of the primary mechanisms for transporting energy from the cool solar surface to the scorching outer corona. EST will simultaneously observe multiple layers of the solar atmosphere, allowing scientists to track these waves in 3D as they propagate upward and deposit their energy.

Key Objectives:

• Trace energy flow: Follow the path of Alfvén and magneto-acoustic waves from the photosphere to the chromosphere.
• Identify heating mechanisms: Determine how these waves dissipate their energy, heating the surrounding plasma.
• High-frequency dynamics: Capture rapid wave oscillations that previous telescopes were too slow to resolve.