Magnetic Effects at the Edge of the Solar System: MHD Instabilities, the de Laval Nozzle Effect, and an Extended Jet
| العنوان: | Magnetic Effects at the Edge of the Solar System: MHD Instabilities, the de Laval Nozzle Effect, and an Extended Jet |
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| المؤلفون: | L. Bettarini, Darren L. DeZeeuw, Ward B. Manchester, Tamas I. Gombosi, Marco Velli, Igor V. Sokolov, M. Opher, P. C. Liewer, Gabor Toth |
| المصدر: | The Astrophysical Journal. 611:575-586 |
| بيانات النشر: | American Astronomical Society, 2004. |
| سنة النشر: | 2004 |
| مصطلحات موضوعية: | Physics, Solar System, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Mechanics, Astrophysics, Magnetic field, Solar wind, Space and Planetary Science, Physics::Space Physics, Solar rotation, Magnetohydrodynamic drive, Magnetohydrodynamics, Heliosphere |
| الوصف: | To model the interaction between the solar wind and the interstellar wind, magnetic fields must be included. Recently Opher et al. 2003 found that, by including the solar magnetic field in a 3D high resolution simulation using the University of Michigan BATS-R-US code, a jet-sheet structure forms beyond the solar wind Termination Shock. Here we present an even higher resolution three-dimensional case where the jet extends for $150AU$ beyond the Termination Shock. We discuss the formation of the jet due to a de Laval nozzle effect and it's su bsequent large period oscillation due to magnetohydrodynamic instabilities. To verify the source of the instability, we also perform a simplified two dimensional-geometry magnetohydrodynamic calculation of a plane fluid jet embedded in a neutral sheet with the profiles taken from our 3D simulation. We find remarkable agreement with the full three-dimensional evolution. We compare both simulations and the temporal evolution of the jet showing that the sinuous mode is the dominant mode that develops into a velocity-shear-instability with a growth rate of $5 \times 10^{-9} sec^{-1}=0.027 years^{-1}$. As a result, the outer edge of the heliosphere presents remarkable dynamics, such as turbulent flows caused by the motion of the jet. Further study, e.g., including neutrals and the tilt of the solar rotation from the magnetic axis, is required before we can definitively address how this outer boundary behaves. Already, however, we can say that the magnetic field effects are a major player in this region changing our previous notion of how the solar system ends. Comment: 24 pages, 13 figures, accepted for publication in Astrophysical Journal (2004) |
| تدمد: | 1538-4357 0004-637X |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::205f61655f88b6920ed186fcbb4fcea9 https://doi.org/10.1086/422165 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....205f61655f88b6920ed186fcbb4fcea9 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 15384357 0004637X |
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