Simulating Solar Maximum Conditions Using the Alfvén Wave Solar Atmosphere Model (AWSoM)

To simulate solar coronal mass ejections (CMEs) and predict their time of arrival and geomagnetic impact, it is important to accurately model the background solar wind conditions in which CMEs propagate. We use the Alfvén Wave Solar atmosphere Model (AWSoM) within the the Space Weather Modeling Framework to simulate solar maximum conditions during two Carrington rotations and produce solar wind background conditions comparable to the observations. We describe the inner boundary conditions for AWSoM using the ADAPT global magnetic maps and validate the simulated results with EUV observations in the low corona and measured plasma parameters at L1 as well as at the position of the Solar Terrestrial Relations Observatory spacecraft. This work complements our prior AWSoM validation study for solar minimum conditions and shows that during periods of higher magnetic activity, AWSoM can reproduce the solar plasma conditions (using properly adjusted photospheric Poynting flux) suitable for providing proper initial conditions for launching CMEs.Fil: Sachdeva, Nishtha. University of Michigan; Estados UnidosFil: Tóth, Gábor. University of Michigan; Estados UnidosFil: Manchester, Ward B.. University of Michigan; Estados UnidosFil: van der Holst, Bart. University of Michigan; Estados UnidosFil: Huang, Zhenguang. University of Michigan; Estados UnidosFil: Sokolov, Igor V.. University of Michigan; Estados UnidosFil: Zhao, Lulu. University of Michigan; Estados UnidosFil: Al Shidi, Qusai. University of Michigan; Estados UnidosFil: Chen, Yuxi. University of Michigan; Estados UnidosFil: Gombosi, Tamas I.. University of Michigan; Estados UnidosFil: Henney, Carl J.. University of Michigan; Estados UnidosFil: Lloveras, Diego Gustavo. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Vasquez, Alberto Marcos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentin

Stormtime Energetics: Energy Transport Across the Magnetopause in a Global MHD Simulation

Funding Information: This research was funded through NSF grant number 2033563 and as part of the NASA DRIVE Center SOLSTICE (Grant Number 80NSSC20K0600). Publisher Copyright: © Copyright © 2021 Brenner, Pulkkinen, Al Shidi and Toth.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 (Formula presented.), flank (Formula presented.), and tail cross section (Formula presented.) 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.Peer reviewe

What sustained multi-disciplinary research can achieve: The space weather modeling framework

Funding Information: Acknowledgements. This work was supported by NASA DRIVE Science Center grant 80NSSC20K0600 and NASA MMS grant 80NSSC19K0564, NASA LWS grants 80NSSC20K0185, 80NSSC20K0190, 80NSSC20K1778 and 80NSSC17K0681, NASA SSW grant 80NSSC20K0854, NASA HSR 80NSSC20K1313, NASA 80NSSC21K0047, the NSF PRE-EVENTS grant 1663800 and NSF SWQU grant PHY-2027555. The authors thank Drs. John Dorelli and Natalia Buzulukova for providing their unpublished result to be shown in the paper (Fig. 15). The authors also thank Ms. Deborah Eddy for making the paper more readable. Publisher Copyright: © T.I. Gombosi et al., Published by EDP Sciences 2021.Magnetohydrodynamics (MHD)-based global space weather models have mostly been developed and maintained at academic institutions. While the "free spirit"approach of academia enables the rapid emergence and testing of new ideas and methods, the lack of long-Term stability and support makes this arrangement very challenging. This paper describes a successful example of a university-based group, the Center of Space Environment Modeling (CSEM) at the University of Michigan, that developed and maintained the Space Weather Modeling Framework (SWMF) and its core element, the BATS-R-US extended MHD code. It took a quarter of a century to develop this capability and reach its present level of maturity that makes it suitable for research use by the space physics community through the Community Coordinated Modeling Center (CCMC) as well as operational use by the NOAA Space Weather Prediction Center (SWPC).Peer reviewe