Driving dynamical inner‐heliosphere models with in situ solar wind observations

Owens, M.J. ORCID: https://orcid.org/0000-0003-2061-2453, Barnard, L. A. ORCID: https://orcid.org/0000-0001-9876-4612, Turner, H. ORCID: https://orcid.org/0000-0002-4012-8004, Gyeltshen, D. ORCID: https://orcid.org/0009-0004-8411-7042, Edward‐Inatimi, N. ORCID: https://orcid.org/0009-0001-6211-5781, O’Donoghue, J. ORCID: https://orcid.org/0000-0002-4218-1191, Lockwood, M. ORCID: https://orcid.org/0000-0002-7397-2172, Watson, S., Rutala, M. ORCID: https://orcid.org/0000-0002-1837-4057, Jackman, C. M. ORCID: https://orcid.org/0000-0003-0635-7361 and Riley, P. ORCID: https://orcid.org/0000-0002-1859-456X (2026) Driving dynamical inner‐heliosphere models with in situ solar wind observations. Space Weather, 24 (1). e2025SW004675. ISSN 1542-7390 doi: 10.1029/2025SW004675

Abstract/Summary

Key Points Inner‐boundary conditions to solar wind models at 0.1 AU can be produced from in situ observations, typically at 1 AU We describe and test methods to account for transient structures, solar wind acceleration and stream interactions between 0.1 and 1 AU This enables quick and accurate reconstruction of inner‐heliosphere structure without the need for magnetograms

Item Type	Article
URI	https://centaur.reading.ac.uk/id/eprint/127815
Identification Number/DOI	10.1029/2025SW004675
Refereed	Yes
Divisions	Science > School of Mathematical, Physical and Computational Sciences > Department of Meteorology
Publisher	American Geophysical Union
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