Planetary ionospheres – sources and dynamic drivers

Abstract

Abstract. External energy inputs into all planetary upper atmospheres (including more than a half dozen moons with atmospheres) are comprised of combinations of solar EUV, soft x-rays, solar energetic particles, solar wind charged particles, magnetospherically accelerated particles, solar wind electric field, interplanetary dust particles as well as propagating lower atmosphere disturbances. Each input has analogous physical interactions with all planetary ionospheres and upper atmospheres, but the integrated consequences of the multiple energy inputs vary from planet to planet. The Earth forms the framework for most fundamental processes because of extensive measurements of the effects of each of the inputs. However the conditions at Earth are far different from those at the carbon dioxide atmosphere of magnetic field-free, slow-rotating Venus, the carbon dioxide atmosphere of Mars with patchy remnant magnetic fields, while the outer planets have hydrogen atmospheres, are fast rotating with intrinsic magnetic fields, and encompass moons that interact with the magnetospheres and have exotic atmospheres. Although the physical processes are known, our understanding of our solar system's ionospheres diminishes with increasing distance from the Sun.

Discovery of Suprathermal Ionospheric Origin Fe+ in and Near Earth's Magnetosphere

“…Such a discussion is beyond the scope of this study, and detailed composition and velocity distribution at numerous altitudes is lacking. Metal layers at other planets are formed by the same universal processes (Benna et al, ; Grebowsky & Aikin, ; Pesnell & Grebowsky, ).…”