In this section
@article{Mendillo:2018:10.1016/j.icarus.2017.12.033,
author = {Mendillo, M and Trovato, J and Moore, L and Mueller-Wodarg, I},
doi = {10.1016/j.icarus.2017.12.033},
journal = {Icarus},
pages = {34--46},
title = {Comparative ionospheres: terrestrial and giant planets},
url = {http://dx.doi.org/10.1016/j.icarus.2017.12.033},
volume = {303},
year = {2018}
}
TY - JOUR
AB - The study of planetary ionospheres within our solar system offers a variety of settings to probe mechanisms of photo-ionization, chemical loss, and plasma transport. Ionospheres are a minor component of upper atmospheres, and thus their mix of ions observed depends on the neutral gas composition of their parent atmospheres. The same solar irradiance (x-rays and extreme-ultra-violet vs. wavelength) impinges upon each of these atmospheres, with solar flux magnitudes changed only by the inverse square of distance from the Sun. If all planets had the same neutral atmosphere—with ionospheres governed by photochemical equilibrium (production=loss)—their peak electron densities would decrease as the inverse of distance from the Sun, and any changes in solar output would exhibit coherent effects throughout the solar system.Here we examine the outer planet with the most observations of its ionosphere (Saturn) and compare its patterns of electron density with those at Earth under the same-day solar conditions. We show that, while the average magnitudes of the major layers of molecular ions at Earth and Saturn are approximately in accord with distance effects, only minor correlations exist between solar effects and day-to-day electron densities. This is in marked contrast to the strong correlations found between the ionospheres of Earth and Mars. Moreover, the variability observed for Saturn's ionosphere (maximum electron density and total electron content) is much larger than found at Earth and Mars. With solar irradiance changes far too small to cause such effects, we use model results to explore the roles of other agents. We find that water sources from Enceladus at low latitudes, and ‘ring rain’ at middle latitudes, contribute substantially to variability via water ion chemistry. Thermospheric winds and electrodynamics generated at auroral latitudes are suggested causes of high latitude ionospheric variability, but remain inconclusive due to the l
AU - Mendillo,M
AU - Trovato,J
AU - Moore,L
AU - Mueller-Wodarg,I
DO - 10.1016/j.icarus.2017.12.033
EP - 46
PY - 2018///
SN - 0019-1035
SP - 34
TI - Comparative ionospheres: terrestrial and giant planets
T2 - Icarus
UR - http://dx.doi.org/10.1016/j.icarus.2017.12.033
UR - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000424534300004&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR - http://hdl.handle.net/10044/1/60815
VL - 303
ER -