The Solar-Stellar Connection

TL;DR

Recent observational, theoretical, and simulation advances have significantly enhanced understanding of stellar convection, rotation, and magnetism, revealing similarities between the Sun and other stars and improving models of stellar magnetohydrodynamics.

Contribution

The paper synthesizes recent progress in observations, theory, and simulations to deepen understanding of stellar magnetism and dynamo processes, highlighting new empirical data and modeling approaches.

Findings

Ensemble asteroseismology constrains stellar rotation and activity.

Large surveys expand parameter space for stellar magnetism studies.

Improved simulations advance understanding of stellar dynamos.

Abstract

We discuss how recent advances in observations, theory and numerical simulations have allowed the stellar community to progress in its understanding of stellar convection, rotation and magnetism and to assess the degree to which the Sun and other stars share similar dynamical properties. Ensemble asteroseismology has become a reality with the advent of large time domain studies, especially from space missions. This new capability has provided improved constraints on stellar rotation and activity, over and above that obtained via traditional techniques such as spectropolarimetry or CaII H&K observations. New data and surveys covering large mass and age ranges have provided a wide parameter space to confront theories of stellar magnetism. These new empirical databases are complemented by theoretical advances and improved multi-D simulations of stellar dynamos. We trace these pathways through which a lucid and more detailed picture of magnetohydrodynamics of solar-like stars is beginning to emerge and discuss future prospects.