HR: 11:05h
AN: SH42A-04    [Abstracts]
TI: Timing of the 2-3 kHz Radio Events Observed by Voyager
AU: * Mitchell, J J
EM: mitchell@physics.usyd.edu.au
AF: School of Physics, A28, University of Sydney, Sydney, NSW 2006 Australia
AU: Cairns, I H
EM: cairns@physics.usyd.edu.au
AF: School of Physics, A28, University of Sydney, Sydney, NSW 2006 Australia
AU: Mueller, H -
EM: Hans-Reinhard.Mueller@dartmouth.edu
AF: Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755 United States
AU: Mueller, H -
EM: Hans-Reinhard.Mueller@dartmouth.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, Riverside, CA 92512 United States
AU: Zank, G P
EM: gary.zank@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, Riverside, CA 92512 United States
AB: Radio emissions observed at 2-3~kHz by the Voyager spacecraft occur when global merged interaction regions (GMIRs) cross the heliopause. The radiation is thought to occur when a GMIR enters a region close to the heliopause where the electron speed distribution is primed with a superthermal tail, produced by lower hybrid drive. Recently, emission mechanisms have been proposed for these events, and subsequent work has confirmed that these mechanisms predict dynamic spectra which closely resemble the steady component observed by the Voyager spacecraft. Here, these results are extended using simulations [Zank and Muller, 2003] in which the solar wind ram pressure varies with the solar cycle. We predict that strong emissions can occur 2-3 years after solar maximum, which is in close agreement with previous observed events.
DE: 7534 Radio emissions
DE: 2162 Solar cycle variations (7536)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting