Timing of the 2-3 kHz Radio Events Observed by Voyager

Details Timing of the 2-3 kHz Radio Events Observed by Voyager Timing of the 2-3 kHz Radio Events Observed by Voyager

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh42a..04m&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH42A-04

Physics

7534 Radio Emissions, 2162 Solar Cycle Variations (7536)

Scientific paper

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.

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