• MODELS - Daily updated results by various driving coronal models (1.7 AU, low-res, 3h cadence, landscape):

• MISSIONS - Daily updated results to support heliospheric missions (5.3 AU, low-res, 3h cadence, landscape):

• ARCHIVE - Animations and temporal profiles in 2011-2014:

• EVENTS - Selected CME events simulated in higher resolution and presented with more details.

• ENLIL solar wind code. The numerical code ENLIL (Sumerian god of wind and storms) is a research tool for simulations of corotating and transient solar wind disturbances. The physical model is based upon the ideal magnetohydrodynamic (MHD) description and the numerical scheme is an explicit high-resolution TVD Lax-Friedrichs scheme.

• IPSBD (UCSD tomography) model data. This model uses observations of the interplanetary scintillation (IPS) from STELab radio arrays to calculate the solar wind density and radial velocity. A tomographic technique and a kinematic model are used to reconstruct the global structure of the solar wind. ENLIL uses output from this model and constructs solar wind source conditions at 0.1 AU. Note that a 6-hour cadence of IPSBD maps are used to drive the simulation.
• Wang-Sheeley-Arge (WSA) model data. This model uses observations of the photospheric magnetic field, potential field source surface (PFSS) and Shatten current sheet (SCS) models, and an empirical formula to derive the radial magnetic field and flow velocity. ENLIL uses output from the WSA model driven by the daily-updated GONG observations and constructs solar wind source conditions at 0.1 AU. WSADU and WSADT labels use a single map (standard approach) and temporal sequence of maps (experimental), respectively.

• Synoptic magnetograms. Remote observations of the magnetic field in the solar photosphere by the GONG Network (six sites around the globe) processed by by the National Solar Observatory (NSO).
• IPS observations. Remote observations of interplanetary scintillations (IPS) by the antenna system (Toyokawa year-round; Fuji, Sugadaira and Kiso from spring to the beginning of winter) operated by the Solar-Terrestrial Environment Laboratory (STELab) of the Nagoya University in Japan.
• CMEs Cone model parameters. Manual operational fitting of coronal mass ejections (CMEs) observed by SOHO/LASCO and/or STEREO/COR coronagraphs using the cone model by CCMC/SWRC staff.
• Trajectories of Planets and Spacecraft. These positions are used during ENLIL computations to store values of the solar wind density, velocity, temperature, and magnetic field, and they are also displayed on the global solar wind plots.
• ACE Real Time Solar Wind. Values of the solar wind density, velocity, temperature, and magnetic field are overlaid on plots showing the evolution of parameters at Earth to indicate the accuracy of the numerical simulation.
• STEREO Real Time Solar Wind. Values of the solar wind density, velocity, temperature, and magnetic field are overlaid on plots showing the evolution of parameters at Stereo A and B spacecraft to indicate the accuracy of the numerical simulation.

Acknowledgments: This work has been supported in part by AFOSR, NASA, and NSF Agencies, and by GMU/SPACS, NASA/CCMC, NOAA/SWPC, RRA/KSWC Institutes.

Last update: 2014-10-14