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

Gombosi, T. I.; Chen, Yuxi; Glocer, A.; Huang, Zhenguang; Jia, Xianzhe; Liemohn, Michael W.; Manchester, W.; Pulkkinen, Tuija; Sachdeva, Nishtha; Shidi, Qusai Al; Соколов, И. В.; Szente, Judit; Tenishev, V.; Tóth, G.; Holst, Bart van der; Welling, D. T.; Zhao, Lulu; Zou, Shasha

doi:10.1051/swsc/2021020

Cited by 55 publications

(48 citation statements)

References 360 publications

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“…The Space Weather Modeling Framework (SWMF) comprises a set numerical models to simulate plasma processes from the Sun to Earth's upper atmosphere and/or the outer heliosphere (Tóth et al, 2012;Gombosi et al, 2021). The simulation core is the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme (BATSRUS), which solves the 3dimensional extended magnetohydrodynamic (MHD) equations in various forms (Powell et al, 1999).…”

Section: Space Weather Modeling Frameworkmentioning

confidence: 99%

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Statistics of geomagnetic storms: Global simulations perspective

Pulkkinen

Brenner²,

Shidi³

et al. 2022

Front. Astron. Space Sci.

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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.

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Section: Space Weather Modeling Frameworkmentioning

confidence: 99%

“…The SWMF and the Geospace configuration numerical schemes are described in detail in (Tóth et al, 2012;Pulkkinen et al, 2013;Gombosi et al, 2021).…”

Section: Space Weather Modeling Frameworkmentioning

confidence: 99%

Statistics of geomagnetic storms: Global simulations perspective

Pulkkinen

Brenner²,

Shidi³

et al. 2022

Front. Astron. Space Sci.

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“…BATS‐R‐US is a global magnetohydrodynamic model that employs ideal single‐fluid MHD equations to describe the solar wind‐magnetosphere‐ionosphere interaction (Powell et al., 1999; Tóth et al., 2012). It is part of the Space Weather Modeling Framework, or SWMF (Gombosi et al., 2021). The equations are solved on a three‐dimensional block‐adaptive Cartesian grid.…”

Section: Magnetohydrodynamic Modelmentioning

confidence: 99%

Tracking the Subsolar Bow Shock and Magnetopause

Sibeck¹,

Silveira

Collier³

2022

JGR Space Physics

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At rest, the magnetopause lies along the locus of points where the sum of the thermal and magnetic pressures in the magnetosheath balance the sum of those same quantities in the magnetosphere. Magnetic pressures generally dominate the total pressure on the magnetospheric side. Pressure imbalances cause the magnetopause to move. When the solar wind dynamic pressure increases, the sum of the thermal and magnetic pressures in the magnetosheath increases proportionally and the dayside magnetopause moves Earthward to a location where an equivalent magnetospheric pressure can be found, that is, a place where dipole magnetic field strengths are greater (Martyn, 1951). When the solar wind dynamic pressure decreases, the dayside magnetopause moves outward to a place where dipolar magnetic field strengths are lower. When solar wind dynamic pressures remain constant but magnetospheric magnetic pressures increase, perhaps in response to enhanced ring current strengths during the main phase of a geomagnetic storm, the dayside magnetopause moves outward at much as 7% to a location some ∼0.7 R E outside its normal position where dipolar magnetic field strengths are weaker and pressure balance can be reestablished (Schield, 1969). When dayside magnetospheric magnetic pressures decrease in response to enhanced Region 1 Birkeland current strengths driven by reconnection and magnetic flux removal from the dayside magnetosphere (Hill & Rassbach, 1975;Maltsev & Lyatsky, 1975), the dayside magnetopause moves inward to a location where the dipole magnetic field strength suffices to restore pressure balance. Magnetotail magnetic field strengths increase during the growth phase of substorms, but decrease abruptly at substorm onset. The corresponding variation in the cross-tail current first weakens but later enhances dayside magnetospheric magnetic field strengths, consistent with inward dayside magnetopause motion during the growth phase but outward motion following substorm onset.There is a specific time scale for magnetopause motion associated with each of the drivers above. The pressure variations associated with solar wind discontinuities transmitted into the magnetosheath propagate antisunward at velocities comparable to those of the solar wind, and consequently require only several minutes to transit the entire dayside magnetosphere. Consistent with this expectation, the rise (or fall) times for the corresponding step function changes in dayside magnetopause location, magnetospheric magnetic field strength, and global current perturbations range from ∼2 to 4 min (Patel & Cahill, 1974). The durations of ring current enhancements are much longer, for the weakest geomagnetic storms on the order of 6 hr, for moderate storms on the order of 30 hr, and for the most intense storms from 12 to 93 hr (Vennerstrøm et al., 2016), These storms can be divided into growth, main, and recovery phases, each lasting from several to many hours, indicating only gradual inflations of the dayside magnetosphere followed by very gradual deflations. Steady...

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“…The Pybats module of Spacepy provides tools for handling output from the Space Weather Modeling Framework (Tóth et al, 2005(Tóth et al, , 2012Gombosi et al, 2021). The SWMF is a framework that executes, synchronizes, and couples together many physics-based domain models of the complex heliosphere system, from solar corona to planetary atmospheres (e.g., Powell et al, 1999;Welling et al, 2015;Mukhopadhyay et al, 2020;Sachdeva et al, 2021).…”

Section: Pybatsmentioning

confidence: 99%

The SpacePy space science package at 12 years

Niehof

Morley²,

Welling³

et al. 2022

Front. Astron. Space Sci.

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For over a decade, the SpacePy project has contributed open-source solutions for the production and analysis of heliophysics data and simulation results. Here we introduce SpacePy’s functionality for the scientific user and present relevant design principles. We examine recent advances and the future of SpacePy in the broader scientific Python ecosystem, concluding with some of the work that has used SpacePy.

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

Cited by 55 publications

References 360 publications

Statistics of geomagnetic storms: Global simulations perspective

Statistics of geomagnetic storms: Global simulations perspective

Tracking the Subsolar Bow Shock and Magnetopause

The SpacePy space science package at 12 years

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