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Spontaneous hot flow anomalies at quasi‐parallel shocks: 2. Hybrid simulations
Author(s) -
Omidi N.,
Zhang H.,
Sibeck D.,
Turner D.
Publication year - 2013
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
eISSN - 2169-9402
pISSN - 2169-9380
DOI - 10.1029/2012ja018099
Subject(s) - foreshock , bow shock (aerodynamics) , physics , magnetosheath , bow wave , solar wind , geophysics , shock (circulatory) , computational physics , shock wave , classification of discontinuities , magnetic field , mechanics , dissipation , magnetohydrodynamics , magnetopause , geology , seismology , medicine , mathematical analysis , mathematics , quantum mechanics , aftershock , thermodynamics
Motivated by recent THEMIS observations, this paper uses 2.5‐D electromagnetic hybrid simulations to investigate the formation of Spontaneous Hot Flow Anomalies (SHFAs) upstream of quasi‐parallel bow shocks during steady solar wind conditions and in the absence of discontinuities. The results show the formation of a large number of structures along and upstream of the quasi‐parallel bow shock. Their outer edges exhibit density and magnetic field enhancements, while their cores exhibit drops in density, magnetic field, solar wind velocity, and enhancements in ion temperature. Using virtual spacecraft in the simulation, we show that the signatures of these structures in the time series data are very similar to those of SHFAs seen in THEMIS data and conclude that they correspond to SHFAs. Examination of the simulation data shows that SHFAs form as the result of foreshock cavitons interacting with the bow shock. Foreshock cavitons in turn form due to the nonlinear evolution of ULF waves generated by the interaction of the solar wind with the backstreaming ions. Because foreshock cavitons are an inherent part of the shock dissipation process, the formation of SHFAs is also an inherent part of the dissipation process leading to a highly nonuniform plasma in the quasi‐parallel magnetosheath including large‐scale density and magnetic field cavities.