HR: 11:35h
AN: SH41C-06 INVITED     [PDF]
TI: Solar Mass Ejection Imager (SMEI) - Hectometric/Kilometric Wave Comparisons
AU: * Bougeret, J
EM: jean-louis.bougeret@obspm.fr
AF: LESIA-CNRS-Observatoire de Paris, 5, place Jules Janssen, Meudon, 92195 France
AB: Radio radiation is commonly produced throughout the interplanetary medium at long wavelengths in the decametric/hectometric/kilometric range. It results from plasma radiation mechanisms involving populations of energetic electrons either accelerated at the Sun --for instance during the solar flares--, or in the interplanetary medium --for instance at the front of interplanetary shocks--. These radio emissions are currently observed by several spacecraft including WIND and ULYSSES. They will be monitored in the near future by programs as STEREO. Several types of radiation have been identified. It is currently understood that the so-called interplanetary type III radio emissions trace large scale structures in the solar wind. The interplanetary type II radio emissions are associated with travelling shock fronts, possibly ahead of Interplanetary Coronal Mass Ejections. Long lasting (several days) storms of type III bursts are associated with solar active regions and may trace large scale corotating interplanetary structures. All these radio observations provide unique information on localized energetic phenomena in the solar wind. The comparison with the Solar Mass Ejection Imager will provide for the first time a unique chance to identify large scale structures in the interplanetary medium, either transient or corotating, that can be associated with radio emissions. In this paper we compare the respective capabilities of the instruments and we discuss a number of open questions for which SMEI - hectometric/kilometric comparisons could provide a clue.
DE: 2102 Corotating streams
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2139 Interplanetary shocks
DE: 7514 Energetic particles (2114)
DE: 7534 Radio emissions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting