Reconnection rates and X line motion at the magnetopause: Global 2D‐3V hybrid‐Vlasov simulation results
| Autor: | Paul Cassak, Minna Palmroth, Urs Ganse, Sanni Hoilijoki, Heli Hietala, Yann Pfau-Kempf, Brian Walsh, Sebastian von Alfthan |
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| Přispěvatelé: | Department of Physics, Space Physics Research Group |
| Rok vydání: | 2017 |
| Předmět: |
010504 meteorology & atmospheric sciences
INTERPLANETARY MAGNETIC-FIELD Motion (geometry) Numerical modeling MAGNETOSHEATH 01 natural sciences Plasma flow Magnetosheath PLASMA-FLOW Physics::Plasma Physics FLUX-TRANSFER EVENTS 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics EARTHS MAGNETOPAUSE Interplanetary magnetic field 010303 astronomy & astrophysics 0105 earth and related environmental sciences Line (formation) Physics hybrid-Vlasov magnetopause MIRROR STRUCTURES Magnetic reconnection Geophysics 115 Astronomy Space science Computational physics MODEL numerical modeling 13. Climate action Space and Planetary Science magnetic reconnection Physics::Space Physics Magnetopause THEMIS OBSERVATIONS CLUSTER OBSERVATIONS DAYSIDE MAGNETOPAUSE |
| Zdroj: | Journal of Geophysical Research: Space Physics |
| ISSN: | 2169-9402 2169-9380 |
| Popis: | We present results from a first study of the local reconnection rate and reconnection site motion in a 2D-3V global magnetospheric self-consistent hybrid-Vlasov simulation with due southward interplanetary magnetic field. We observe magnetic reconnection at multiple locations at the dayside magnetopause and the existence of magnetic islands, which are the 2-D representations of flux transfer events. The reconnection locations (the X lines) propagate over significant distances along the magnetopause, and reconnection does not reach a steady state. We calculate the reconnection rate at the location of the X lines and find a good correlation with an analytical model of local 2-D asymmetric reconnection. We find that despite the solar wind conditions being constant, the reconnection rate and location of the X lines are highly variable. These variations are caused by magnetosheath fluctuations, the effects of neighboring X lines, and the motion of passing magnetic islands. |
| Databáze: | OpenAIRE |
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