Home > Research > Publications & Outputs > Trapped Particle Motion in Magnetodisk Fields

Electronic data

  • final

    Rights statement: Accepted for publication in Journal of Geophysical Research: Space Physics. Copyright 2020 American Geophysical Union. Further reproduction or electronic distribution is not permitted.

    Accepted author manuscript, 3.79 MB, PDF document

    Available under license: CC BY-NC: Creative Commons Attribution-NonCommercial 4.0 International License


Text available via DOI:

View graph of relations

Trapped Particle Motion in Magnetodisk Fields

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Article numbere2020JA027827
<mark>Journal publication date</mark>1/07/2020
<mark>Journal</mark>Journal of Geophysical Research: Space Physics
Issue number7
Number of pages18
Publication StatusPublished
<mark>Original language</mark>English


The spatial and temporal characterization of trapped charged particle trajectories in magnetospheres has been extensively studied in dipole magnetic field structures. Such studies have allowed the calculation of spatial quantities, such as equatorial loss cone size as a function of radial distance, the location of the mirror points along particular field lines (L‐shells) as a function of the particle's equatorial pitch angle, and temporal quantities such as the bounce period and drift period as a function of the radial distance and the particle's pitch angle at the equator. In this study, we present analogous calculations for the disk‐like field structure associated with the giant rotation‐dominated magnetospheres of Jupiter and Saturn as described by the University College London/Achilleos‐Guio‐Arridge (UCL/AGA) magnetodisk model. We discuss the effect of the magnetodisk field on various particle parameters and make a comparison with the analogous motion in a dipole field. The bounce period in a magnetodisk field is in general smaller the larger the equatorial distance and pitch angle, by a factor as large as ∼8 for Jupiter and ∼2.5 for Saturn. Similarly, the drift period is generally smaller, by a factor as large as ∼2.2 for equatorial distances ∼20–24 RJ at Jupiter and ∼1.5 for equatorial distances ∼7–11 RS at Saturn.