Journal article
Quasilinear Wave‐Particle Analysis in the Source Region of Jovian Kilometric Radio Emission
Journal of geophysical research. Space physics, Vol.130(11), e2025JA034328
11/2025
DOI: 10.1029/2025JA034328
Abstract
Jovian broadband kilometric emission (bKOM) is observed by the Juno spacecraft within a source region in the northern hemisphere near the equatorward edge of the auroral oval. A well‐developed upward loss cone is the free‐energy source of the bKOM. The spacecraft also detected intense low‐energy (few hundred eV) counter‐streaming electrons which are known to generate whistler mode emission via Landau resonance. In addition, hot protons (tens of keV thermal energy) accompanied by Alfvénic low‐frequency emissions are also frequently detected in these source regions. We use quasilinear analysis to examine the generation and growth of bKOM and the dynamics of wave‐particle interaction of the electron beams with bKOM and the growth of whistler mode and Z‐mode emission. We also carry out quasilinear analysis of protons interacting with the low‐frequency modes that coexist in the bKOM source region. The comprehensive quasilinear wave‐particle analysis involving the energetic loss‐cone electrons and high‐frequency bKOM emission, counter‐streaming electron beams and low‐frequency/low‐intensity electrostatic modes, and hot protons and Alfvén/proton‐cyclotron wave emission, are shown to be successful in explaining/replicating the observed wave emission characteristics and various charged‐particle properties.
Radio emission at kilometric wavelengths in the frequency range 20–500 kHz, known as the Jovian broadband kilometric emission (bKOM), is detected by the Juno space probe as it travels around the planet Jupiter, in the region close to the giant planet's polar region. Energetic electrons executing gyration motion around Jupiter's strong magnetic field are observed together with electrons primarily streaming back and forth along the field. Hot protons are also pervasively detected in the same region. A mathematical analysis to explain how these electrons reconfigure their motions while giving off the EM radiation as well as other types of EM signals that exist within the Jupiter's magnetosphere is carried out. It is found that the kinetic energy associated with those electrons primarily executing the gyro motion is partially radiated away as high‐frequency bKOM emission, while the electrons moving back and forth along the magnetic field also lose some of their kinetic energy, which is converted to a low‐intensity electrostatic signals. The hot protons, on the other hand, are shown to be responsible for generating low‐frequency EM signals, which are also measured by instruments onboard Juno spacecraft.
Upward‐traveling electron loss‐cone distribution together with counter streaming electron beam and hot protons are detected in bKOM source region Kilometric emission is measured accompanied by ion‐cyclotron frequency range emission and weak whistler mode‐like signature The observed wave spectra and particle characteristics are modeled by employing quasilinear wave‐particle analysis
Details
- Title: Subtitle
- Quasilinear Wave‐Particle Analysis in the Source Region of Jovian Kilometric Radio Emission
- Creators
- P. H. Yoon - University of Maryland, College ParkJ. D. Menietti - University of IowaF. Allegrini - The University of Texas at San AntonioW. S. Kurth - University of IowaJ. B. Faden - University of IowaG. B. Hospodarsky - University of IowaJ. E. P. Connerney - Space Research Corporation Annapolis MD USAS. J. Bolton - Southwest Research Institute
- Resource Type
- Journal article
- Publication Details
- Journal of geophysical research. Space physics, Vol.130(11), e2025JA034328
- DOI
- 10.1029/2025JA034328
- ISSN
- 2169-9380
- eISSN
- 2169-9402
- Publisher
- Wiley
- Grant note
- NSF: 2203321 Planetary Science Division: 80NSSC23K0662 Department of Energy: DOE DE-SC0022963 University of Maryland: Z6536201 NASA New Frontiers Program: 699041X
The authors wish to thank J. Chrisinger for help with some of the figures and L. Granroth who established the zenodo archive. P. H. Y. was supported by NASA Grant 80NSSC23K0662, NSF Grant 2203321, and the Department of Energy (DOE DE-SC0022963) through the NSF/DOE Partnership in Basic Plasma Science and Engineering. JDM acknowledges support from subcontract Z6536201 to the University of Maryland. Research conducted at the University of Iowa was supported by NASA New Frontiers Program through Contract 699041X with Southwest Research Institute. F. A. was funded by NASA New Frontiers Program for Juno. We acknowledge the use of the Space Physics Data Repository at the University of Iowa supported by the Roy J. Carver Charitable Trust.
- Language
- English
- Date published
- 11/2025
- Academic Unit
- Physics and Astronomy
- Record Identifier
- 9985027357802771
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