HR: 1340h
AN: SM53B-1281    [Abstracts]
TI: Jovian millisecond-bursts as markers of Alfvenic electron acceleration
AU: * Mottez, F
EM: fabrice.mottez@obspm.fr
AF: LUTH, Observatoire de Paris, CNRS, Universite Paris Diderot, 5 Place Jules Janssen, Meudon, 92190, France
AU: Hess, S
EM: sebastien.hess@obspm.fr
AF: LUTH, Observatoire de Paris, CNRS, Universite Paris Diderot, 5 Place Jules Janssen, Meudon, 92190, France
AU: Hess, S
EM: sebastien.hess@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 Place Jules Janssen, Meudon, 92190, France
AU: Zarka, P
EM: philippe.zarka@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 Place Jules Janssen, Meudon, 92190, France
AB: Jupiter's radio emissions are dominated in intensity by decametric radio emissions due to the Io-Jupiter interaction. Previous analyses suggest that these emissions are cyclotron-maser emissions in the flux tubes connecting Io's wake to Jupiter, triggered by electrons accelerated from Io to Jupiter. We present simulations of a hot electron population under the assumption of acceleration by Alfvén waves in the Io flux tube. Outside of limited acceleration regions where parallel electric field associated with Alfvén waves are found, the electrons have an adiabatic motion along the magnetic field lines. Electron distribution functions are computed at various altitudes and times (relatively to the propagation of the Alfvén wave). Near Jupiter, a loss cone appears in the magnetically mirrored electron population; it amplifies extraordinary (X) mode radio waves. The X-mode growth rate (depending on time and altitude) is computed, and a theoretical dynamic spectrum of the resulting Jovian radio emissions is built. This spectrum is compared with those made from observations.
DE: 6219 Io
DE: 6939 Magnetospheric physics (2700)
DE: 7534 Radio emissions
DE: 7815 Electrostatic structures
DE: 7845 Particle acceleration
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting