Magnetic connectivity in the time-dependent corona and heliosphere

Lionello, R. ORCID: https://orcid.org/0000-0001-9231-045X, Downs, C. ORCID: https://orcid.org/0000-0003-1759-4354, Mason, E. I. ORCID: https://orcid.org/0000-0002-8767-7182, Linker, J. A. ORCID: https://orcid.org/0000-0003-1662-3328, Riley, P. ORCID: https://orcid.org/0000-0002-1859-456X and Owens, M. J. ORCID: https://orcid.org/0000-0003-2061-2453 (2026) Magnetic connectivity in the time-dependent corona and heliosphere. The Astrophysical Journal Letters, 1001 (1). L23. ISSN 2041-8205 doi: 10.3847/2041-8213/ae5791

Abstract/Summary

Abstract Magnetic flux fills the heliosphere, expands outward from the solar corona, and is fundamentally related to the structure and dynamics of the solar corona and solar wind. Open magnetic flux and the fast wind are thought to originate from open magnetic field lines in coronal holes. Less understood processes in the streamer belt and the boundaries of coronal holes, associated with the more variable slow wind, may be formed by interchange reconnection between open and closed magnetic flux. Interchange reconnection is thought to give rise to field lines that are “folded,” i.e., that turn back on themselves. The properties of strahl electrons measured in the solar wind give clues to the heliospheric magnetic connectivity. Unidirectionally outward strahl indicates open field lines, while bidirectional strahl is associated with closed magnetic flux and coronal mass ejections (CMEs). Inward-directed, unidirectional strahl is believed to indicate folded flux. We use two time-dependent, flux-evolutionary magnetohydrodynamic (MHD) models of the combined corona and heliosphere, one for a solar-minimum configuration and one for the 2024 total solar eclipse, to investigate the magnetic connectivity of the corona/heliosphere system. We examine how magnetic connectivity varies with distance from the Sun in the two configurations. We evaluate the evolutionary effects by contrasting time-dependent results with the corresponding steady-state calculations and compare the model connectivities with statistical studies of strahl. The connectivities in the time-evolving simulations are roughly consistent with observed strahl occurrence rates, while those from the steady-state models are not. Our results suggest that complex magnetic connectivities are ubiquitous in the heliosphere.

Item Type	Article
URI	https://centaur.reading.ac.uk/id/eprint/129317
Identification Number/DOI	10.3847/2041-8213/ae5791
Refereed	Yes
Divisions	Science > School of Mathematical, Physical and Computational Sciences > Department of Meteorology
Publisher	IOP Science
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