Fundamentals of impulsive energy release in the corona

TL;DR

Understanding impulsive energy release in the solar corona requires coordinated multi-wavelength observations during solar maximum, focusing on magnetic reconnection, particle acceleration, and energy transport to address key open questions.

Contribution

This paper emphasizes the importance of coordinated observations during solar cycle 26 to advance understanding of impulsive energy release mechanisms in the corona.

Findings

Identifies key open questions about energy release in the corona.

Highlights the need for multi-wavelength, co-optimized observations.

Suggests a flagship or combined mission approach for comprehensive study.

Abstract

It is essential that there be coordinated and co-optimized observations in X-rays, gamma-rays, and EUV during the peak of solar cycle 26 (~2036) to significantly advance our understanding of impulsive energy release in the corona. The open questions include: What are the physical origins of space-weather events? How are particles accelerated at the Sun? How is impulsively released energy transported throughout the solar atmosphere? How is the solar corona heated? Many of the processes involved in triggering, driving, and sustaining solar eruptive events -- including magnetic reconnection, particle acceleration, plasma heating, and energy transport in magnetized plasmas -- also play important roles in phenomena throughout the Universe. This set of observations can be achieved through a single flagship mission or, with foreplanning, through a combination of major missions (e.g., the previously proposed FIERCE mission concept).