Magnetic activity in cool stars: manifestations and relevance to exoplanets

arXiv:2606.31617 · astro-ph.SR, astro-ph.EP · Submitted 2026-06-30 · Read on arXiv

E. Işık, A. Valio, A. Strugarek, S. Järvinen, K. Vida, A. Buccino, K. Namekata, T. Hackman, J. Alvarado-Gomez, D. Nandy, A. O. Farrish, K. Poppenhäger, P. Figueira

astro-ph.SR, astro-ph.EP

Submitted: 2026-06-30

Comments: 86 pages, submitted to Space Science Reviews. Abstract abridged. Comments are welcome

Code: https://github.com/Transit-Model-CRAAM/pipelineMCMC

License: http://creativecommons.org/licenses/by-nc-nd/4.0/

The gist: Understanding stellar magnetic activity is central to exoplanet science in two ways: it sets the dynamic astrospheric boundary condition governing planetary space environments, and it is the primary

Terminology

Abstract

Understanding stellar magnetic activity is central to exoplanet science in two ways: it sets the dynamic astrospheric boundary condition governing planetary space environments, and it is the primary obstacle to exoplanet detection and characterisation, since magnetically driven variability imprints correlated quasi-periodic signals across detection time series. In cool stars, MHD-dynamo-generated fields emerge at the photosphere as bipolar regions, drive chromospheric and coronal heating, modulate irradiance and wind, and power flares and coronal mass ejections. Spatial scales range from individual flux tubes to global coronal configurations, and temporal scales from minutes to decades and beyond, requiring observational and theoretical tools of correspondingly wide scope. We review observational manifestations and physical models of magnetic activity in stars with outer convective envelopes, addressed to the exoplanet community. We develop the solar-stellar connection through the 'Sun in Time' framework and a sequence of solar analogues serving as evolutionary snapshots of a solar-mass star over several Gyr. We survey photospheric, chromospheric, and coronal activity diagnostics across timescales, together with forward-modelling tools translating surface field distributions into signals at or above the level of exoplanet detection. Empirical rotation-activity relationships and their physical interpretation are examined across all three atmospheric layers. Surface reconstruction techniques are assessed for their diagnostic reach and limitations. The evolution of magnetism in solar-like stars is discussed as context for habitability and as a window to other worlds. We close with an account of how stellar magnetism sculpts the astrospheric environment and affects close-in exoplanets, followed by a synthesis of outstanding issues and an outlook on future prospects.

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