Magnetopause Reconnection and Indents Induced by Foreshock Turbulence
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2021-05-31
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Citation of Original Publication
Chen, Li-Jen et al.; Magnetopause Reconnection and Indents Induced by Foreshock Turbulence; Geophysical Research Letters, 48, 11, 31 May, 2021; https://doi.org/10.1029/2021GL093029
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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
Public Domain Mark 1.0
This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract
Abstract
Based on global hybrid simulation results, we predict that foreshock turbulence can reach the magnetopause and lead to reconnection as well as Earth-sized indents. Both the interplanetary magnetic field (IMF) and solar wind are constant in our simulation, and hence, all dynamics are generated by foreshock instabilities. The IMF in the simulation is mostly Sun-Earth aligned with a weak northward and zero dawn-dusk component, such that subsolar magnetopause reconnection is not expected without foreshock turbulence modifying the magnetosheath fields. We show a reconnection example to illustrate that the turbulence can create large magnetic shear angles across the magnetopause to induce local bursty reconnection. Magnetopause reconnection and indents developed from the impact of foreshock turbulence can potentially contribute to dayside loss of planetary plasmas.
Plain Language Summary
Turbulence structures are commonly generated as ions reflected by planetary bow shocks interact with the incoming solar wind. We use a large-scale simulation treating ions as particles and electrons as a fluid to investigate the impact of these turbulence structures on the magnetopsheres. Based on the simulation results, we predict that the turbulence can open magnetic field lines on the dayside and lead to planet-sized indents. Our work unfolds a potential pathway through which planetary plasmas can escape to the upstream solar wind.