HR: 0800h
AN: SM31A-1200    [Abstracts]
TI: Observations of Earth's Bow Shock Structure from the First Chinese scientific Satellite, Double Star
AU: * Parks, G K
EM: parks@ssl.berkeley.edy
AF: Space Sciences Laboratory, UC Berkeley, Berkeley, CA 94720 United States
AU: Dandouras, I
EM: dandouras@cesr.fr
AF: CESR, Avenue de Colonel, Toulouse, 31029 France
AU: Wilber, M
EM: wilber@ssl.berkeley.edu
AF: University of California, Space Sciences Laboratory, Berkeley, 94720 United States
AU: Meziane, K
AF: Physics Department, University of New Brunswick, New Brunswick, 12345 Canada
AU: Cao, B
AF: CSSAR, Chinese Academy of Sciences, Beijing, 12345 China
AU: Reme, H
AF: CESR, Avenue de Colonel, Toulouse, 31029 France
AU: Sauvaud, J
AF: CESR, Avenue de Colonel, Toulouse, 31029 France
AU: Bosqued, J
AF: CESR, Avenue de Colonel, Toulouse, 31029 France
AU: Mazelle, C
AF: CESR, Avenue de Colonel, Toulouse, 31029 France
AU: Bavassano-Cattaneo, M B
AF: IFSI, Rome, Rome, 12345 Italy
AU: Fazakerly, A
AF: MSSL, Holmbury St. Mary, Surrey, 12345 United Kingdom
AU: Goldstein, M
AF: GSFC, Greenbelt Rd., Greenbelt, MD 20771 United States
AU: Lucek, E
AF: Blackett Laboratory, Imperial College, London, 12345 United Kingdom
AU: Balogh, A
AF: Blackett Laboratory, Imperial College, London, 12345 United Kingdom
AU: Escoubet, P
AF: ESTEC, European Space Agency, Noordwijk, 12345 Netherlands
AB: New features of Earth's bow shock structure have been observed by the HIA ion experiment on the first Chinese scientific satellite, Double Star. At times of coincident apogee, the Cluster spacecraft served as monitors of the upstream condition providing information from nearly identical instruments. The combination of the orbit with an apogee approximately at 13.5 Re and data obtained in high time resolution (4s) has permitted observations of the shock structure with unprecendented detail. We present examples of laminar and turbulent shocks observed in late February and early March (2004) when the Double Star apogee was located on the sunward side skimming the shock boundary. This talk will discuss (1) evolutionary features of ion distributions of the solar wind slowdown converting almost the entire flow energy into thermal energy, (2) microscopic features that could be signifying kinetic processes at work and (3) ordering of density, bulk velocity and temperature to show the distribution of solar wind momentum and energy throughout the shock transition.
DE: 2109 Discontinuities
DE: 2139 Interplanetary shocks
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting