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Extended magnetohydrodynamics with embedded particle-in-cell simulation of Ganymede's magnetosphere
KTH, Skolan för datavetenskap och kommunikation (CSC), Beräkningsvetenskap och beräkningsteknik (CST).ORCID-id: 0000-0003-0639-0639
KTH, Skolan för datavetenskap och kommunikation (CSC), Beräkningsvetenskap och beräkningsteknik (CST).
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2016 (Engelska)Ingår i: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 121, nr 2, s. 1273-1293Artikel i tidskrift (Refereegranskat) Published
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Abstract [en]

We have recently developed a new modeling capability to embed the implicit particle-in-cell (PIC) model iPIC3D into the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme magnetohydrodynamic (MHD) model. The MHD with embedded PIC domains (MHD-EPIC) algorithm is a two-way coupled kinetic-fluid model. As one of the very first applications of the MHD-EPIC algorithm, we simulate the interaction between Jupiter's magnetospheric plasma and Ganymede's magnetosphere. We compare the MHD-EPIC simulations with pure Hall MHD simulations and compare both model results with Galileo observations to assess the importance of kinetic effects in controlling the configuration and dynamics of Ganymede's magnetosphere. We find that the Hall MHD and MHD-EPIC solutions are qualitatively similar, but there are significant quantitative differences. In particular, the density and pressure inside the magnetosphere show different distributions. For our baseline grid resolution the PIC solution is more dynamic than the Hall MHD simulation and it compares significantly better with the Galileo magnetic measurements than the Hall MHD solution. The power spectra of the observed and simulated magnetic field fluctuations agree extremely well for the MHD-EPIC model. The MHD-EPIC simulation also produced a few flux transfer events (FTEs) that have magnetic signatures very similar to an observed event. The simulation shows that the FTEs often exhibit complex 3-D structures with their orientations changing substantially between the equatorial plane and the Galileo trajectory, which explains the magnetic signatures observed during the magnetopause crossings. The computational cost of the MHD-EPIC simulation was only about 4 times more than that of the Hall MHD simulation. Key Points

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American Geophysical Union (AGU), 2016. Vol. 121, nr 2, s. 1273-1293
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kinetic simulation, Ganymede, Hall MHD, Galileo
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URN: urn:nbn:se:kth:diva-185660DOI: 10.1002/2015JA021997ISI: 000373002100024Scopus ID: 2-s2.0-84959142207OAI: oai:DiVA.org:kth-185660DiVA, id: diva2:923451
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QC 20160426

Tillgänglig från: 2016-04-26 Skapad: 2016-04-25 Senast uppdaterad: 2017-11-30Bibliografiskt granskad

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Markidis, Stefano

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Markidis, StefanoPeng, Ivy Bo
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