Abstract
AbstractObservations of equatorial magnetosonic waves made during the Cluster Inner Magnetospheric Campaign clearly show discrete spectra consisting of emissions around harmonics of the proton gyrofrequency. Equatorial magnetosonic waves are important because of their ability to efficiently scatter electrons in energy and pitch angle. This wave‐particle interaction is numerically modeled through the use of diffusion coefficients, calculated based on a continuous spectrum such as that observed by spectrum analyzers. Using the Chirikov overlap resonance criterion, the calculation of the diffusion coefficient will be assessed to determine whether they should be calculated based on the discrete spectral features as opposed to a continuous spectrum. For the period studied, it is determined that the discrete nature of the waves does fulfill the Chirikov overlap criterion and so the use of quasi‐linear theory with the assumption of a continuous frequency spectrum is valid for the calculation of diffusion coefficients.
Highlights
The understanding of the evolution of relativistic fluxes within the outer radiation belt is important for mitigation of deep surface charging effects on spacecraft hardware
Equatorial magnetosonic waves are important because of their ability to efficiently scatter electrons in energy and pitch angle. This wave-particle interaction is numerically modeled through the use of diffusion coefficients, calculated based on a continuous spectrum such as that observed by spectrum analyzers
A number of numerical codes, such as VERB (Versatile Electron Radiation Belt) [Shprits et al, 2008, 2009] or PADIE (Pitch Angle and Energy Diffusion of Ions and Electrons) [Glauert and Horne, 2005], have been developed to model the dynamics of relativistic electrons within the radiation belts. These codes are based on the solution of a set of diffusion equations and require tensors of the quasi-linear diffusion coefficients to account for particle interaction with various wave modes
Summary
The understanding of the evolution of relativistic fluxes within the outer radiation belt is important for mitigation of deep surface charging effects on spacecraft hardware. A number of numerical codes, such as VERB (Versatile Electron Radiation Belt) [Shprits et al, 2008, 2009] or PADIE (Pitch Angle and Energy Diffusion of Ions and Electrons) [Glauert and Horne, 2005], have been developed to model the dynamics of relativistic electrons within the radiation belts. These codes are based on the solution of a set of diffusion equations and require tensors of the quasi-linear diffusion coefficients to account for particle interaction with various wave modes. The main types of waves that should be taken into account are chorus, hiss, equatorial magnetosonic waves (EMWs), and electromagnetic ion cyclotron waves
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
