Modeling

The AMIE procedure is an optimally constrained, weighted least-squares fit of electric potential distribution to diverse types of atmospheric observations. Knowledge of these distributions is important in many areas of magnetospheric, ionospheric, and thermospheric physics.

The Coupled Magnetosphere Ionosphere Thermosphere (CMIT) model consists of the Lyon-Fedder-Mobarry (LFM) model of the magnetosphere coupled to the Thermosphere-Ionosphere-Electrodynamics General Circulation Model (TIE-GCM). Together, these provide a comprehensive description of the response of the geospace system to variations in the solar wind and the interplanetary magnetic field.

DOCFM is an NCAR/CfA collaboration that is funded by AFOSR to model the global coronal magnetic field using magnetometric and other observations, with the goal of improving space weather forecasts of magnetic orientation within coronal mass ejections.

This set of codes is intended to be used for forward modeling of various coronal observables, and for accessing and comparing to existing data. 

The GLobal airglOW model, also known as GLOW, is a toolkit of subroutines and driver programs for performing calculations of optical emissions in the upper atmosphere, particularly the thermosphere and ionosphere, above about 100 km altitude.

A Numerical Model of Planetary Waves and Solar Tides in the Earth's Atmosphere.

The LFM Code is an integrated simulation model for the global magnetosphere-ionosphere system. The heart of the model is a time-dependent, ideal MHD calculation of the state of the magnetosphere.

Output from Matthias Rempel's sunspot model.

The High Altitude Observatory at the National Center for Atmospheric Research has developed a series of numeric simulation models of the Earth's upper atmosphere, including the upper Stratosphere, Mesosphere, and Thermosphere.

The Whole Atmosphere Community Climate Model with thermosphere and ionosphere extension (WACCM-X) is a comprehensive numerical model, spanning the range of altitude from the Earth’s surface to the upper thermosphere.

The main objective of our focussed science team is to take joint effort to develop the most comprehensive, dynamically consistent picture possible of solar velocities at the surface, in the convection zone and tachocline, and determine the MHD effects induced by these motions, by building and/or employing MHD models capable of operating in data-driven and data-assimilative modes.