Magnetic connectivity from the Sun to the Earth with MHD models I. Impact of the magnetic modelling for connectivity validation

Abstract

This article discusses the magnetic connectivity between the Sun and the Earth, which is essential for understanding solar wind and space weather events. Due to limited direct observations, reliable simulations are necessary. The most commonly used method is the two-step ballistic method, but it has many free parameters that affect the results. The authors propose a method based on self-consistent magnetohydrodynamic (MHD) models. They combine the COCONUT coronal model with the EUHFORIA heliospheric model to compute magnetic field lines from the Earth to the Sun and quantify spatial and temporal uncertainties. To validate their method, they analyze four events associated with high-speed streams from well-identified coronal holes. The results show partial overlap with the assumed coronal holes of origin, ranging from 19% to 100% depending on the event. They also examine the magnetic polarity observed on Earth, finding that MHD simulations provide a good polarity estimation, with agreement ranging from 36% to 69% across the events. Spatial and temporal uncertainties explain the mixed results for some cases. MHD models appear more effective during periods of maximum solar activity due to the latitudinal extent of the heliospheric current sheet (HCS). The authors conclude that MHD models offer results as good as the two-step ballistic method, with potential for improvement as more critical physics are integrated into the models.

11 pages, 6 figures, accepted in A&A

References in corpus (11)

• Understanding space weather to shield society: A global road map for 2015-2025 commissioned by COSPAR and ILWS
• Origins of the Ambient Solar Wind: Implications for Space Weather
• Magnetic connectivity of the ecliptic plane within 0.5 AU : PFSS modeling of the first PSP encounter
• Properties and geoeffectiveness of solar wind high-speed streams and stream interaction regions during solar cycles 23 and 24
• Prediction and Verification of Parker Solar Probe Solar Wind Sources at 13.3 R${}_{\odot }$
• COCONUT, a novel fast-converging MHD model for solar corona simulations: II. Assessing the impact of the input magnetic map on space-weather forecasting at minimum of activity
• The Observational Uncertainty of Coronal Hole Boundaries in Automated Detection Schemes
• Constraining Global Coronal Models with Multiple Independent Observables
• Observational Evidence of S-Web Source of the Slow Solar Wind
• Effects of Mesh Topology on MHD Solution Features in Coronal Simulations
• To E or not to E: Numerical Nuances of Global Coronal Models

Cited by in corpus (1)

• Physics-Based Simulation of the 2013 April 11 Solar Energetic Particle Event