Ion Precipitation Into Io's Poles Driven by a Strong Sub‐Alfvénic Interaction-Reference-Cited by-同舟云学术

Ion Precipitation Into Io's Poles Driven by a Strong Sub‐Alfvénic Interaction

Published:2024-07-29 Issue:15 Volume:51 Page:
ISSN:0094-8276
Container-title:Geophysical Research Letters
language:en
Short-container-title:Geophysical Research Letters

Author:

Szalay J. R.¹^ORCID,Saur J.²^ORCID,Allegrini F.³⁴^ORCID,Ebert R. W.³⁴^ORCID,Valek P. W.²^ORCID,Clark G.⁵^ORCID,Accetta K.¹,Bagenal F.⁶^ORCID,Bolton S. J.³^ORCID,Damiano P.⁷^ORCID,Dols V.⁶^ORCID,Mauk B.⁵^ORCID,McComas D. J.¹^ORCID,Paranicas C.⁵^ORCID,Sarkango Y.¹^ORCID,Strobel D.⁸^ORCID,Sulaiman A. H.⁹^ORCID,Wilson R. J.⁶^ORCID

Affiliation:

1. Department of Astrophysical Sciences Princeton University Princeton NJ USA

2. Institute of Geophysics and Meteorology University of Cologne Cologne Germany

3. Southwest Research Institute San Antonio TX USA

4. Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA

5. The Johns Hopkins University Applied Physics Laboratory Laurel MD USA

6. Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder CO USA

7. University of Alaska Fairbanks Fairbanks AK USA

8. The Johns Hopkins University Baltimore MD USA

9. University of Minnesota Minneapolis MN USA

Abstract

AbstractJuno performed two close flybys of Io and found enhanced field‐aligned proton fluxes are absorbed by Io. These protons are absorbed at mass input rates comparable to previous estimates for hydrogen losses from Io, hence Jupiter is likely the source of hydrogen at Io. The conditions necessary for this to occur are: (a) formation of Alfvén waves at Io, (b) wave‐particle coupling to energize protons, (c) anti‐planetward transport of ions due to the magnetic mirror force and/or parallel acceleration, and (d) strong sub‐Alfvénic interaction slowing the flow connected to Io's fluxtube allowing for sufficient travel time for energized ions to transit to Io. The derived slowdown of ≤12% the upstream value is linked to filamentation within the Alfvén wing. This mechanism is likely operating at all strongly interacting satellites and provides an avenue to transfer material from a planetary body to its satellites, including exoplanets and brown dwarfs.

Funder

Planetary Science Division

Horizon 2020 Framework Programme

National Aeronautics and Space Administration

University of Colorado

Southwest Research Institute

Publisher

American Geophysical Union (AGU)

Link

https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2024GL110205

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