HR: 1340h
AN: SA33A-1129 [Abstracts]
TI: Global Distribution of the Equatorial Plasma Bubbles in the Premidnight Sector During Solar Maximum as
Observed by KOMPSAT-1
AU: * PARK, J
EM: jhpark@space.kaist.ac.kr
AF: KAIST, Department of physics, KAIST, Daejeon, 305-701
Korea, Republic of
AU: MIN, K
EM: kwmin@space.kaist.ac.kr
AF: KAIST, Department of physics, KAIST, Daejeon, 305-701
Korea, Republic of
AU: KIM, V P
EM: kimvp@izmiran.rssi.ru
AF: IZMIRAN, IZMIRAN, Triotsk, 142190
Russian Federation
AU: KIL, H
EM: hyosub.kil@jhuapl.edu
AF: APL, Johns Hopkins University, Laurel, MD 20723
United States
AU: LEE, J
EM: jjlee@ssl.berkeley.edu
AF: SSL, U.C. Berkeley, Berkeley, CA 94704
United States
AU: KIM, H
EM: hjkim@space.kaist.ac.kr
AF: KAIST, Department of physics, KAIST, Daejeon, 305-701
Korea, Republic of
AU: LEE, E
EM: eslee@ssl.berkeley.edu
AF: SSL, U.C. Berkeley, Berkeley, CA 94704
United States
AU: LEE, D
EM: dylee@chungbuk.ac.kr
AF: Department of Astronomy and space science, Chungbuk National University, Cheongju, 361-763
Korea, Republic of
AB:
We investigated the global distribution of the equatorial plasma bubbles (EPBs) using the in-situ ion density measurements
from Korea Multi-Purpose Satellite-1 (KOMPSAT-1) at the altitude of 680 km at 2230 LT during the solar maximum period from
June 2000 to August 2001. EPBs were observed at all longitudes around the magnetic dip equator in the equinoctial seasons
with the peak occurrence in the American-Atlantic-African regions. During the northern summer the EPBs occurred predominantly
in the magnetic north in the Indian and west Pacific regions, whereas they are totally suppressed in the American-Atlantic
sectors. During the northern winter the EPBs are highly promoted in the America-Atlantic sectors but are suppressed in other
longitude sectors, especially, in the Pacific sector. We investigated the growth conditions of the Rayleigh-Taylor
instability by using the model atmosphere (MSIS) and ionosphere (IRI). The simulation results show that the global EPB
distribution can be explained by using the upward plasma drift velocity at post-sunset time weighted by the flux-tube
integrated electron content in the lower F region.
DE: 2400 IONOSPHERE
DE: 2415 Equatorial ionosphere
DE: 2439 Ionospheric irregularities
DE: 2447 Modeling and forecasting
DE: 2481 Topside ionosphere
SC: SPA-Aeronomy [SA]
MN: 2004 AGU Fall Meeting