Modelling the peak of the ionospheric E-layer |
| |
| Institution: | 1. Dept. of Electrical and Electronics Engineering, Bilkent University, Turkey;2. Dept. of Electrical and Electronics Engineering, Hacettepe University, Turkey;1. Space Research Institute of the Russian Academy of Sciences, Russia;2. National Research Nuclear University MEPhI, Russia;3. Moscow Institute of Physics and Technology (State University), Russia;4. MPI für Sonnensystemforschung, Germany;1. Institute of Space Science, National Central University, Chung-Li, Taiwan;2. Center for Space and Remote Sensing Research, National Central University, Chung-Li, Taiwan;3. National Space Program Origination, Hsin-Chu, Taiwan;4. Department of Earth Science, National Cheng Kung University, Tainan, Taiwan;1. Faculty of Physics, Sofia University, 1164 Sofia, Bulgaria;2. IGAM, Institute of Physics, University of Graz, 8010 Graz, Austria;3. Abastumani Astrophysical Observatory at Ilia State University, 0162 Tbilisi, Georgia;4. Space Research Institute, Austrian Academy of Sciences, 8042 Graz, Austria;5. Catholic University of America, Washington, DC 20064, USA;6. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;7. Visiting, Department of Geosciences, Tel Aviv University, Ramat-Aviv, Tel Aviv 69978, Israel;8. Department of Physics, DSB Campus, Kumaun University, Nainital 263 001, India |
| |
| Abstract: | Calculations with a full time-varying model are used to study changes in the height and density of the E-layer peak, caused by known changes in the neutral atmosphere. Agreement with mean observed values of NmE requires an increase of 10% in calculated ion densities, and an increase of 33% in the solar-maximum EUV model at λ<150 Å. At a fixed site, changes with the solar zenith angle χ agree well with the simple Chapman theory during most of the daylight hours. Simple modifications to the Chapman equations give improved accuracy near sunrise and sunset. When corrected for changes in χ, model results for summer and equinox show a decrease in the peak density NmE at increasing latitudes. The overall change agrees well with experimental data, as summarised in the IRI model. Known changes in the neutral atmosphere also reproduce the increase in NmE in winter, at latitudes up to 30°. The continuing increase at higher winter latitudes, in the IRI model, requires a major reduction in NO densities in winter. A suitable compromise is suggested. Equations fitted to the model results then provide a simpler and better behaved replacement for the IRI equations. Calculations at night show that known sources of ionisation, largely from starlight, can produce observed peak densities using current chemistry. There is an appreciable change with latitude, as starlight production increases in the southern hemisphere. The improbably large solar cycle change built into the IRI model, at night, cannot be reproduced and is not found in recent data. A new, simpler model is suggested. Changes in zenith angle and atmospheric composition cause the peak height (hmE) to vary between 105 and 120 km, as a function of time, latitude, season and solar flux. These changes are approximated by simple equations that should be definitely preferable over the single, fixed height used in the IRI models. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
