ADAPT/HMI Global Solar Magnetic Maps

Monday, 14 December 2015
Poster Hall (Moscone South)
Carl J Henney1, Charles Nickolos Arge2, Kathleen Shurkin3, Alicia K. Schooley4, Kyle S. Hickmann5 and Humberto C Godinez5, (1)AFRL, Kirtland AFB, NM, United States, (2)Air Force Research Laboratory Kirtland AFB, Kirtland AFB, NM, United States, (3)Boston College, ISR, Chestnut Hill, MA, United States, (4)University of Michigan Ann Arbor, AOSS, Ann Arbor, MI, United States, (5)Los Alamos National Laboratory, Los Alamos, NM, United States
Global solar magnetic maps are the primary input to coronal and heliospheric models used to estimate geoeffective space weather events. The ADAPT (Air Force Data Assimilative Photospheric flux Transport) model has recently been modified to utilize line-of-sight magnetograms observed from the Helioseismic and Magnetic Imager (HMI) to create global flux distribution maps. Compared to ground-based observations, data assimilation of inferred photospheric magnetic field data close to the solar limb is possible as a result of the high quality of HMI magnetograms. Estimation of the global magnetic field distribution continues to be challenging, however, since less than half of the solar surface is viewable via spectropolarimetric measurements at any given time. The lack of farside solar magnetic field observations results in temporal and spatial discontinuities within the global maps at the east-limb boundary (where the observational time difference is greater than two weeks and continuously present) and at the poles (where quality observations are not available for each pole for ~5 months, once per year). In this presentation, we will discuss the progress towards improved data assimilation, modeling the evolution of active regions and polar fields, incorporating helioseismic farside and full-Stokes vector data, and forecasting the solar wind, F10.7 (i.e., the solar 10.7 cm radio flux), and extreme ultraviolet (EUV) irradiance.