HR: 0800h
AN: SM21B-0366    [Abstracts]
TI: Multi-point Observations of the Waveform and Propagation of Lion Roars
AU: * Yearby, K H
EM: k.yearby@sheffield.ac.uk
AF: University of Sheffield, Mappin Street, Sheffield, S1 3JD United Kingdom
AU: Walker, S
EM: simon.walker@sheffield.ac.uk
AF: University of Sheffield, Mappin Street, Sheffield, S1 3JD United Kingdom
AU: Alleyne, H
EM: h.alleyne@sheffield.ac.uk
AF: University of Sheffield, Mappin Street, Sheffield, S1 3JD United Kingdom
AU: Cornilleau-Wehrlin, N
EM: nicole.cornilleau@cetp.ipsl.fr
AF: CETP/IPSL, 10-12 Av. de l'Europe, Velizy, Paris, 78140 France
AU: Maksimovic, M
EM: milan.maksimovic@obspm.fr
AF: Observatoire de Paris, Meudon, Paris, 92195 France
AU: Lahiff, A
EM: adl@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT United Kingdom
AU: Fazakerley, A
EM: anf@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT United Kingdom
AB: Lion roars are intense, short duration packets of whistler mode waves, observed in the magnetosheath. They are typically seen coincident with the magnetic field minima of mirror mode waves. In this study, lion roar activity was observed simultaneously on the four Cluster spacecraft and on the Double Star equatorial (TC1) spacecraft. The Cluster spacecraft were in a tetrahedron formation with approximately 1500km separation, whilst TC1 was 30000km from Cluster, all in the magnetosheath, allowing multi-scale observations of the waves within mirror mode structures. The propagation direction determined from the lion roar waveform measured by the STAFF tri-axial search coil magnetometer is compared to the background magnetic field, and the electron temperature anisotropy estimated from the lion roar frequency ratios is compared to PEACE electron measurements.
DE: 2728 Magnetosheath
DE: 2772 Plasma waves and instabilities (2471)
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005