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Hunt et al Published on-line (16 July 2019).pdf (1.4 MB)

Currents Associated With Saturn's Intra-D Ring Azimuthal Field Perturbations

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journal contribution
posted on 2019-08-21, 09:16 authored by GJ Hunt, SWH Cowley, G Provan, H Cao, EJ Bunce, MK Dougherty, DJ Southwood
During the final 22 full revolutions of the Cassini mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low-latitude current system via the associated azimuthal perturbation field peaking typically at ~10–30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field-aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field-aligned current densities above the ionosphere are typically ~5–10 nA/m2, more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field-aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north-south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller-scale structures, possibly due to rapid temporal or local time variations.

Funding

Work at Imperial College was supported by STFC grant ST/N000692/1. Work at the University of Leicester was supported by STFC grant ST/N000749/1. E. J. B. is supported by a Royal Society Wolfson Research Merit Award. M. K. D. is funded by Royal Society Research Professorship RP140004. H. C. is funded by the Cassini project through NASA Jet Propulsion Laboratory contract 1579625. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data.

History

Citation

Journal of Geophysical Research: Space Physics, 2019, 124

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Journal of Geophysical Research: Space Physics

Publisher

American Geophysical Union (AGU), Wiley

issn

2169-9380

eissn

2169-9402

Acceptance date

2019-07-08

Copyright date

2019

Publisher version

https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2019JA026588

Notes

Calibrated magnetic field data from the Cassini mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).;The file associated with this record is under embargo until 6 months after publication, in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.

Language

en

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