Global Solar Magnetic Maps using Reverse Active Region Modeling
Abstract
Progress toward generating smoothly evolving global solar magnetic maps will be presented, highlighting modifications to the ADAPT (Air Force Data Assimilative Photospheric flux Transport) model to assimilate reverse-modeled far-side flux estimates for newly emerged active regions using east-limb HMI (Helioseismic and Magnetic Imager) vector data. Global solar magnetic maps, which provide estimates of the solar photospheric magnetic field distribution, are the primary input data driver of coronal and heliospheric models. Though full-disk solar magnetograms are now typically available with high temporal cadence, estimating the global magnetic field distribution continues to be a challenge since less than half of the solar surface is viewable with spectropolarimetric measurements at any given moment in time. The absence of solar far-side magnetic field observations and lack of quality polar data result in temporal and spatial discontinuities within global maps at the east-limb boundary and at the poles. Accounting for differential rotation, together with meridional and supergranulation flows, the flux transport component of ADAPT evolves an ensemble of realizations to match the observation time of magnetograph input data before assimilation. For the past five years, the ADAPT model has been operating continuously in a prototype mode at the National Solar Observatory (NSO), generating global photospheric magnetic maps in near real-time. Input to the ADAPT model includes photospheric magnetograms from the NISP (NSO Integrated Synoptic Program) ground-based instruments, GONG (Global Oscillation Network Group) and VSM (Vector SpectroMagnetograph). More recently, the ADAPT model has been updated to utilize line-of-sight and vector magnetograms from HMI. This presentation includes results generated by the WSA (Wang-Sheeley-Arge) model driven by ADAPT global maps that include reverse active region modeling. The benefits of including far-side flux evolution will be reviewed, along with the expected implications when full-disk vector magnetograms of the far-side become available from the Polarimetric and Helioseismic Imager (PHI) on Solar Orbiter.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2018
- Bibcode:
- 2018AGUFMSH43D..38H
- Keywords:
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- 7509 Corona;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMYDE: 7511 Coronal holes;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMYDE: 7524 Magnetic fields;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMYDE: 7924 Forecasting;
- SPACE WEATHER