The excitation of the far ultraviolet electroglow emissions on Uranus, Saturn, and Jupiter.
We propose that the diffuse FUV emissions of H and H2 in excess of photoelectron excitation observed from the sunlit atmospheres of Uranus, Saturn, and Jupiter are produced by electric field acceleration of photoelectrons and ions locally in the upper atmospheres.  This in situ acceleration is required to satisfy the many observational constraints on the altitude distribution, exciting particle energy, and total input energy requirements of the electroglow mechanism.  We further suggest that a primary mechanism leading to this  acceleration is an ionospheric dynamo, which is created in the same manner as the Earth's dynamo.  The calculated altitude of charge separation by the neutral wind drag on ions across magnetic field lines is consistent with the observed peaks in electroglow emissions from the Voyager ultraviolet spectrometer limb scan data on both Saturn (near the homopause) and Uranus (just above the homopause).  This dynamo action therefore appears to initiate the acceleration process, which must have the form of field-aligned potentials to accelerate the magnetized electrons.  We propose that these field-aligned potentials are due to anomalous resistivity, which results from sufficiently high field-aligned currents in the ionosphere to generate plasma instabilities and therefore runaway electrons and ions above some critical lower initial energy.  There are multiple candidate processes for inducing these currents, including polarization in the equivalent F regions and inner magnetospheric convection, and each of these processes should exhibit latitudinal structure.  The acceleration of low-energy electrons in an H2 atmosphere preferentially results in FUV radiation and further ionization, whereas electron acceleration in a nitrogen/oxygen atmosphere such as the Earth's is dominated by elastic scattering and thus results in electric currents.  Individual electron and proton collisions with H2 molecules will result in excitation, ionization, and heating, so that considerable enhancement of the ionospheric density and heating of the upper atmosphere will accompany the FUV emission.
Clarke
J T
JT
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA.
Hudson
M K
MK
Yung
Y L
YL
D004583:Electrons; D019471:Elementary Particle Interactions; D005118:Extraterrestrial Environment; D006859:Hydrogen / Q000032:analysis; D018538:Jupiter; D009584:Nitrogen / Q000032:analysis; D009686:Nuclear Physics; D010100:Oxygen / Q000032:analysis; D011522:Protons; D018539:Saturn; D013056:Spectrophotometry, Ultraviolet / Q000379:methods*; D018540:Uranus
D011522:Protons; D006859:Hydrogen; D009584:Nitrogen; D010100:Oxygen