HR: 1340h
AN: SA33A-1136    [Abstracts]
TI: The correlation between Solar EUV Flux and Plasma Characteristics in the Low-Latitude Topside Ionosphere at Nighttime
AU: * Kim, H
EM: hjkim@space.kaist.ac.kr
AF: Dep. of Physics, KAIST, 373-1 Guseong-dong, Yuseong-gu, Daejeon, 305-701 Korea, Republic of
AU: Park, J
EM: jhpark@space.kaist.ac.kr
AF: Dep. of Physics, KAIST, 373-1 Guseong-dong, Yuseong-gu, Daejeon, 305-701 Korea, Republic of
AU: Min, K
EM: kwmin@space.kaist.ac.kr
AF: Dep. of Physics, KAIST, 373-1 Guseong-dong, Yuseong-gu, Daejeon, 305-701 Korea, Republic of
AU: Lee, J
EM: jjlee@ssl.berkeley.edu
AF: SSL, U. C. Berkeley, Berkeley, CA 94720 United States
AU: Lee, E
EM: eslee@ssl.berkeley.edu
AF: SSL, U. C. Berkeley, Berkeley, CA 94720 United States
AB: We present the results of the correlation between solar EUV flux and ionospheric plasma parameters observed by KOMPSAT-1(685Km altitude, 2250 local time) and DMSP F-15(840Km altitude, 2130 local time) in the low-latitude topside ionosphere. The plasma density and temperature observed by KOMPSAT-1 and DMSP F-15 from June 28, 2000 to August 1, 2001 were analyzed with F10.7 which is a standard proxy for solar EUV flux. Especially, the data of the geomagnetic latitude between -60›r"­ and 60›r"­ in the nighttime were considered at the low- and mid-latitude region. From the result, it was shown that the plasma density and temperature at local maximum density region in the geomagnetic equator were increased with F10.7. Furthermore, the best correlation between F10.7 with a lag of 2 days and plasma parameters was observed. It means that the ionospheric equatorial plasma is influenced by the solar EUV flux with the delay of 2 days.
DE: 2400 IONOSPHERE
DE: 2415 Equatorial ionosphere
DE: 2467 Plasma temperature and density
DE: 2479 Solar radiation and cosmic ray effects
DE: 2481 Topside ionosphere
SC: SPA-Aeronomy [SA]
MN: 2004 AGU Fall Meeting