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In recent years, there has been remarkable progress in solar and heliospheric physics, driven by advancements in observation, theory, and numerical modeling. Breakthrough results from missions such as Solar Orbiter, Parker Solar Probe, CHASE, ASO-S, Aditya-L1, PUNCH, and Proba-3, and from ground-based observatories such as DKIST, have deepened our understanding of solar atmospheric heating, flare-producing eruptions, solar wind acceleration, and the dynamic coupling between the Sun and the heliosphere. Numerical codes such as MURaM, Bifrost, Mancha, RAMENS, R2D2, WholeSun, and SAMS have been developed or are under development to simulate various physical processes in the different layers of the solar atmosphere. However, a fully self-consistent numerical model that spans the entire solar atmosphere and beyond has yet to be achieved. This session aims to provide a platform for researchers to share their latest findings on a variety of topics, including observational studies, numerical simulations, and theory. This session will place special emphasis on numerical modeling approaches and observations, which illuminate the physical processes governing the dynamical activity events in the solar atmosphere, and on the evolution of long-term solar research, which has provided critical insights into solar cycles and variability. We encourage submissions on not only core solar and heliospheric physics topics, but also on topics from related fields, such as magnetospheric, planetary, and stellar physics. By fostering interdisciplinary dialogue, we hope to stimulate new collaborations and insights that will advance our understanding of the Sun and its influence in the solar system. Contributions from early-career researchers and established experts are welcome, and we look forward to vibrant discussions that reflect the diversity and dynamism of this rapidly evolving area of investigation.