HR: 11:40h
AN: SH42A-06    [Abstracts]
TI: Persistent Asymmetries in the Magnetic Field Near Mars
AU: * Crider, D H
EM: crider@cua.edu
AF: Catholic University of America, 620 Michigan Ave., NE, Washington, DC 20064 United States
AU: Brain, D A
EM: brain@ssl.berkeley.edu
AF: Space Science Laboratory, 7 Gauss Way University of California, Berkeley, CA 9 United States
AU: Krymskii, A M
EM: amkrym@yahoo.com
AF: Catholic University of America, 620 Michigan Ave., NE, Washington, DC 20064 United States
AU: Krymskii, A M
EM: amkrym@yahoo.com
AF: Rostov State University, Rostov State University, Rostov-on-Don, 344090 Russian Federation
AU: Breus, T K
EM: breus36@mail.ru
AF: Catholic University of America, 620 Michigan Ave., NE, Washington, DC 20064 United States
AU: Breus, T K
EM: breus36@mail.ru
AF: IKI, Academy of Sciences, Moscow, 117997 Russian Federation
AU: Acuna, M H
EM: mario.acuna@nasa.gov
AF: Goddard Space Flight Center, Code 695, Greenbelt, MD 20771 United States
AU: Halekas, J S
EM: jazzman@ssl.berkeley.edu
AF: Space Science Laboratory, 7 Gauss Way University of California, Berkeley, CA 9 United States
AB: The data from the Mars Global Surveyor MAG/ER demonstrate that the magnetic fields observed near Mars are different from what is expected in the case of standard draping of the Interplanetary Magnetic Field (IMF) around a non-magnetic body. In the draping picture, the draped magnetic fields alternate polarity following IMF polarity. One can expect parity when looking at data from long periods. Meanwhile there is an excess of one polarity near Mars. We discuss the processes that may be responsible for producing the asymmetric distribution of magnetic field in the near-Mars environment.
DE: 2780 Solar wind interactions with unmagnetized bodies
DE: 5440 Magnetic fields and magnetism
DE: 6225 Mars
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005