Join The Team

Team title: Global Solar Magnetic Field Working Team 

Team ID: S2-03

Team Leads:

Carl Henney (Air Force Research Laboratory (AFRL), USA),

Nick Arge (NASA GSFC, USA), 

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Keywords (impact): Climate, Satellite/debris drag, Navigation/CommunicationKeywords (activity type): Understanding , Requirements , Modeling, Forecasting , Data Utilization , Assessment 


The Global Solar Magnetic Field Working Team will address the key challenges and limitations of creating global solar magnetic field maps. In preparation of Solar Orbiter PHI magnetograph data, the team will compare different map generation techniques and different input data sources (e.g., NSO/GONG, SDO/HMI, and SO/PHI), along with how best to combine differing methods and data sources (i.e., vector and LOS, along with different instruments) to improve estimates of the global radial 
magnetic field distribution. The working team will address numerous key questions, for example: How best to estimate poorly observed polar regions when creating global maps? How best to minimize the discontinuity between ~13-day old and newly observed data? How best to propagate global map uncertainties to the coronal & solar wind models? How best to include far-side estimation of magnetic activity from helioseimology (i.e., when not directly observed by SO/PHI)?
How best to validate and quantify success for an ensemble of global maps (i.e., model and observation comparison of, e.g., solar wind parameters, coronal hole boundaries, global mean, or coronal topology)?


  • The working team objective will include detailed comparisons of global magentic maps generated for periods of interest, selecting validation metrics, and evaluating current techniques needed to create realistic estimates of the global photospheric field distribution with uncertainties. Potentially generate a real-time comparison board (using TBD metrics, e.g., global and polar mean stability) of available global maps.
  • Action topics:

Action topics:

  • Definition and quantification of uncertainties in magnetic flux for different solar regions (e.g. poles, active regions, quiet sun),
  • Definition of metrics and validation for coronal structures,
  • Quantification of uncertainties in mapping to solar wind sources

Clusters with overlapping topics: 

S2: Ambient solar magnetic field, heating and spectral irradiance,

H1: Heliospheric magnetic field and solar wind,

H2: CME structure, evolution and propagation through heliosphere

Link to team external website: