Radio Emissions from the Outer Heliosphere

Details Radio Emissions from the Outer Heliosphere Radio Emissions from the Outer Heliosphere

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ssrv...78...53g&link_type=abstract

Space Science Reviews, Volume 78, Issue 1-2, pp. 53-66

Computer Science

19

Heliospheric Radio Emissions, Heliosphere, Heliopause, Termination Shock

Scientific paper

For nearly fifteen years the Voyager 1 and 2 spacecraft have been detecting an unusual radio emission in the outer heliosphere in the frequency range from about 2 to 3 kHz, Two major events have been observed, the first in 1983 84 and the second in 1992 93. In both cases the onset of the radio emission occurred about 400 days after a period of intense solar activity, the first in mid-July 1982, and the second in May June 1991. These two periods of solar activity produced the two deepest cosmic ray Forbush decreases ever observed. Forbush decreases are indicative of a system of strong shocks and associated disturbances propagating outward through the heliosphere. The radio emission is believed to have been produced when this system of shocks and disturbances interacted with one of the outer boundaries of the heliosphere, most likely in the vicinity of the the heliopause. The emission is believed to be generated by the shock-driven Langmuir-wave mode conversion mechanism, which produces radiation at the plasma frequency (f p ) and at twice the plasma frequency (2f p ). From the 400-day travel time and the known speed of the shocks, the distance to the interaction region can be computed, and is estimated to be in the range from about 110 to 160 AU.

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