Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sa31a10r&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SA31A-10
Other
2479 Solar Radiation And Cosmic Ray Effects, 2481 Topside Ionosphere
Scientific paper
We previously reported that there is a 27-day variation in the plasma density and temperature observed by the DMSP spacecraft at 840 km altitude. At the peak of the previous solar cycle (1989 - 1991) the density variation was 40-50%, and the electron temperature (Te) variation was approximately 20% in the evening sector. The variations decreased with decreasing solar activity to near the threshold of detectability (a few percent) of the DMSP instruments. Since the minimum of the solar cycle (1995 - 1997), the variations have increased strongly with the increase in solar activity. Herein, we examine why the variations observed at 840 km altitude are smaller in the sun-lit morning topside ionosphere than in the post-sunset evening topside ionosphere. Also, we will compare the variations with both the standard 10.7 cm radio flux proxy for the solar EUV and with alternative proxies. One alternative proxy is based on satellite drag and the other is based on spectral lines in the visible and near UV portions of the solar spectrum. This comparison shows that the alternative proxies correlate better with the topside ionosphere variations than the 10.7 cm flux. This implies that they are better proxies for the solar EUV. Since the topside ionosphere tends to be coupled with the plasmasphere, we will explore the possibility that there is a similar 27 day variation in the plasmasphere.
Rich Frederic J.
Sultan Peter J.
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