Determining the Mode, Frequency, and Azimuthal Wave Number of ULF Waves During a HSS and Moderate Geomagnetic Storm. Issue 8 (18th August 2018)

• Record Type: Journal Article
• Authors: Murphy, Kyle R.; Inglis, Andrew R.; Sibeck, David G.; Rae, I. Jonathan; Watt, Clare E. J.; Silveira, Marcos; Plaschke, Ferdinand; Claudepierre, Seth G.; Nakamura, Rumi
• Is Part Of: Journal of geophysical research. Volume 123:Issue 8(2018)
• Page Start: 6457
• Page End: 6477
• Publication Date: 2018-08-18
• Subjects: ULF waves -- azimuthal wave number -- mode structure -- geomagnetic storms -- radiation belts; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1029/2017JA024877
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract: Ultralow frequency (ULF) waves play a fundamental role in the dynamics of the inner magnetosphere and outer radiation belt during geomagnetic storms. Broadband ULF wave power can transport energetic electrons via radial diffusion, and discrete ULF wave power can energize electrons through a resonant interaction. Using observations from the Magnetospheric Multiscale mission, we characterize the evolution of ULF waves during a high‐speed solar wind stream (HSS) and moderate geomagnetic storm while there is an enhancement of the outer radiation belt. The Automated Flare Inference of Oscillations code is used to distinguish discrete ULF wave power from broadband wave power during the HSS. During periods of discrete wave power and utilizing the close separation of the Magnetospheric Multiscale spacecraft, we estimate the toroidal mode ULF azimuthal wave number throughout the geomagnetic storm. We concentrate on the toroidal mode as the HSS compresses the dayside magnetosphere resulting in an asymmetric magnetic field topology where toroidal mode waves can interact with energetic electrons. Analysis of the mode structure and wave numbers demonstrates that the generation of the observed ULF waves is a combination of externally driven waves, via the Kelvin‐Helmholtz instability, and internally driven waves, via unstable ion distributions. Further analysis of the periods and toroidal azimuthal wave numbers suggests that these waves can couple with the core electron radiation belt population via the drift resonance during the storm. The azimuthal wave number and structure of ULF wave power (broadband or discrete) have important implications for the inner magnetospheric and radiation belt dynamics. Key Points: ULF wave power is systematically characterized as discrete or broadband, and the azimuthal wave number of discrete ULF waves is determined Storm time discrete ULF waves can couple with the core radiation belt electron population via the drift resonance Storm time ULF waves are the result of both external (Kelvin‐Helmholtz) and internal (plasma instabilities) generation mechanisms