On the Growth and Development of Non-linear Kelvin-Helmholtz Instability at Mars: MAVEN Observations
Loading...
Author/Creator ORCID
Date
2021-08-06
Type of Work
Department
Program
Citation of Original Publication
Poh, Gangkai et al.; On the Growth and Development of Non-linear Kelvin-Helmholtz Instability at Mars: MAVEN Observations; Journal of Geophysical Research : Space Physics, 6 August, 2021; https://doi.org/10.1029/2021JA029224
Rights
This item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
©2021. American Geophysical Union. All Rights Reserved
Access to this item will begin on 2022-02-06
©2021. American Geophysical Union. All Rights Reserved
Access to this item will begin on 2022-02-06
Subjects
Abstract
In this study, we have analyzed MAVEN observations of fields and plasma signatures associated with an encounter of fully-developed Kelvin–Helmholtz (K–H) vortices at the northern polar terminator along Mars’ induced magnetosphere boundary. The signatures of the K–H vortices event are: (i) quasi-periodic, “bipolar-like” sawtooth magnetic field perturbations, (ii) corresponding density decrease, (iii) tailward enhancement of plasma velocity for both protons and heavy ions, (iv) co-existence of magnetosheath and planetary plasma in the region prior to the sawtooth magnetic field signature (i.e. mixing region of the vortex structure), and (v) pressure enhancement (minimum) at the edge (center) of the sawtooth magnetic field signature. Our results strongly support the scenario for the non-linear growth of K–H instability along Mars’ induced magnetosphere boundary, where a plasma flow difference between the magnetosheath and induced-magnetospheric plasma is expected. Our findings are also in good agreement with 3-dimensional local magnetohydrodynamics (MHD) simulation results. MAVEN observations of protons with energies greater than 10 keV and results from the Walén analyses suggests the possibility of particle energization within the mixing region of the K–H vortex structure via magnetic reconnection, secondary instabilities or other turbulent processes. We estimate the lower limit on the K–H instability linear growth rate to be ∼5.84 x 10⁻³ s⁻¹. For these vortices, we estimate the instantaneous atmospheric ion escape flux due to the detachment of plasma clouds during the late non-linear stage of K–H instability to be ∼5.90 x 10²⁶ particles/s. Extrapolation of loss rates integrated across time and space will require further work.