Coupling between the solar wind and magnetosphere can be expressed in terms of energy transfer through the separating boundary known as the magnetopause. Geospace simulation is performed using the Space Weather Modeling Framework (SWMF) of a multi-ICME impact event on February 18–20, 2014 in order to study the energy transfer through the magnetopause during storm conditions. The magnetopause boundary is identified using a modified plasma β and fully closed field line criteria to a downstream distance of −20Re. Observations from Geotail, Themis, and Cluster are used as well as the Shue 1998 model to verify the simulation field data results and magnetopause boundary location. Once the boundary is identified, energy transfer is calculated in terms of total energy flux K, Poynting flux S, and hydrodynamic flux H. Surface motion effects are considered and the regional distribution of energy transfer on the magnetopause surface is explored in terms of dayside X>0, flank X<0, and tail cross section X=Xmin regions. It is found that total integrated energy flux over the boundary is nearly balanced between injection and escape, and flank contributions dominate the Poynting flux injection. Poynting flux dominates net energy input, while hydrodynamic flux dominates energy output. Surface fluctuations contribute significantly to net energy transfer and comparison with the Shue model reveals varying levels of cylindrical asymmetry in the magnetopause flank throughout the event. Finally existing energy coupling proxies such as the Akasofu ϵ parameter and Newell coupling function are compared with the energy transfer results.

We use the Space Weather Modeling Framework Geospace configuration to simulate a total of 122 storms from the period 2010–2019. With the focus on the storm main phase, each storm period was run for 54 hr starting from 6 hr prior to the start of the Dst depression. The simulation output of ground magnetic variations, ΔBH in particular, were compared with ground magnetometer station data provided by SuperMAG to statistically assess the Geospace model regional magnetic perturbation prediction performance. Our results show that the regional predictions at mid‐latitudes are quite accurate, but the high‐latitude regional disturbances are still difficult to predict.

We present results of 131 geomagnetic storm simulations using the University of Michigan Space Weather Modeling Framework Geospace configuration. We compare the geomagnetic indices derived from the simulation with those observed, and use 2D cuts in the noon-midnight planes to compare the magnetopause locations with empirical models. We identify the location of the current sheet center and look at the plasma parameters to deduce tail dynamics. We show that the simulation produces geomagnetic index distributions similar to those observed, and that their relationship to the solar wind driver is similar to that observed. While the magnitudes of the Dst and polar cap potentials are close to those observed, the simulated AL index is consistently underestimated. Analysis of the magnetopause position reveals that the subsolar position agrees well with an empirical model, but that the tail flaring in the simulation is much smaller than that in the empirical model. The magnetotail and ring currents are closely correlated with the Dst index, and reveal a strong contribution of the tail current beyond 8 RE to the Dst index during the storm main phase.

No abstract

&lt;p&gt;Energy transport into and throughout Earth&#039;s magnetosphere has direct consequences for human infrastructure in orbit and on the planets surface but studying the entire system in a comprehensive and quantifiable way has many challenges. In this work we use the Space Weather Modeling Framework (SWMF) in the Geospace configuration with the addition of the Conductance Model for Extreme Events (CMEE) to simulate a real storm event and take a thorough look at the energy content within regions of the magnetosphere. The magnetosphere outer boundary is defined using techniques published in Brenner et al. 2021 and is represented in the simulation domain as an iso-surface. Additional boundaries between the lobes and the closed field line plasma sheet are then determined in order to study the transport of energy between the different plasma regimes from the magnetosheath to the inner magnetosphere. The results are shown as time-series of integrated energy content within each region volume, and integrated energy flux between the regional interfaces. These volume energies and surface fluxes are compared with input solar wind conditions, storm phases, and empirical solar wind - magnetosphere coupling functions. Finally, the results are quantitatively assessed in terms of statistical parameters of the integrated quantities during each storm phase as well as statistical relationships such as correlation coefficients between energy from the sheath to the lobes and lobes to the closed field line region.&amp;#160;&lt;/p&gt;