Driving dynamical inner-heliosphere models with in-situ solar-wind observations
Reconstruction of inner-heliosphere conditions is typically a three-step process. 1, the photospheric magnetic field is used to constrain a coronal model, which provides an estimate of the steady-state solar-wind at 0.1 AU; 2, coronagraph observations
Authors
- Pete Riley (ORCID: https://orcid.org/0000-0002-1859-456X)
- James O’Donoghue (ORCID: https://orcid.org/0000-0002-4218-1191)
- Luke Barnard (ORCID: https://orcid.org/0000-0001-9876-4612)
- M. J. Owens (ORCID: https://orcid.org/0000-0003-2061-2453)
- Sarah Watson (ORCID: https://orcid.org/0000-0003-4534-8783)
- C. M. Jackman (ORCID: https://orcid.org/0000-0003-0635-7361)
- M. Lockwood (ORCID: https://orcid.org/0000-0002-7397-2172)
- Harriet Turner (ORCID: https://orcid.org/0000-0002-4012-8004)
- Matthew Rutala (ORCID: https://orcid.org/0000-0002-1837-4057)
- Nathaniel Oputari Edward-Inatimi
- Dechen Lhamo Gyeltshen
Institutions
- Dublin Institute For Advanced Studies (IE)
- Predictive Science (United States) (US)
- University of Reading (GB)
Publication Details
- Published
- 2025-08-18
- DOI
- https://doi.org/10.22541/essoar.175553624.46922203/v1
- Primary Topic
- Solar and Space Plasma Dynamics
- Type
- article
- Field-Weighted Citation Impact
- 0.00