HR: 1340h
AN: SH43A-1140 [Abstracts]
TI: Large-Scale Magnetic Field Convection and Flux Ropes in the Ionospheres of Mars and Venus
AU: Krymskii, A M
EM: amkrym@yahoo.com
AF: Catholic University of America, Department of Physics
620 Michigan Ave, NE, Washington, DC 20064
United States
AU: Krymskii, A M
EM: amkrym@yahoo.com
AF: Rostov State University, 5 Zorge St., Rostov-on-Don, CA 344090
Russian Federation
AU: Ness, N F
EM: nfnudel@yahoo.com
AF: Catholic University of America, Department of Physics
620 Michigan Ave, NE, Washington, DC 20064
United States
AU: * Crider, D H
EM: crider@cua.edu
AF: Catholic University of America, Department of Physics
620 Michigan Ave, NE, Washington, DC 20064
United States
AU: Breus, T K
EM: breus36@mail.ru
AF: Catholic University of America, Department of Physics
620 Michigan Ave, NE, Washington, DC 20064
United States
AU: Breus, T K
EM: breus36@mail.ru
AF: IKI, Russian Academy of Sciences, Moscow, MD 117997
Russian Federation
AU: Acuna, M H
EM: mario.h.acuna@nasa.gov
AF: NASA GSFC, Code 695, Greenbelt, MD 20771
United States
AU: Bojkov, D I
SH43A-1140
AF: Rostov State University, 5 Zorge St., Rostov-on-Don, CA 344090
Russian Federation
AB:
The pattern of the magnetic field/plasma convection can be, to some extent, recovered from the magnetic field measurements by
employing either theoretical or numerical models. Pioneer-Venus Orbiter magnetic field measurements have been used to study
large-scale convection-diffusion of the interplanetary magnetic fields in the Venusian day-side ionosphere and formation of
flux ropes. For the sake of comparison, we use the MAG/ER day-time measurements of the magnetic field at the altitudes from
90 to 180 km during the elliptical orbits of MGS. Analysis of the altitude variation of the characteristics of the
large-scale magnetic fields, which were measured away from the crustal magnetic anomalies, is summarized. The low density of
the Martian atmosphere together with the crustal magnetization results in remarkable differences of the magnetic field
features within the ionosphere of Venus and Mars (even in its Venus-like northern hemisphere where the crustal magnetization
is, on average, low). Various scenarios of flux ropes formation and evolution are discussed in order to explain why only a
few flux ropes were observed deep inside the subsolar ionosphere of Mars.
DE: 2459 Planetary ionospheres (5435, 5729, 6026)
DE: 2780 Solar wind interactions with unmagnetized bodies
DE: 5421 Interactions with particles and fields
DE: 6225 Mars
DE: 6295 Venus
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005