Recent observations and analyses of heliospheric 2-3 kHz radio emissions

Details Recent observations and analyses of heliospheric 2-3 kHz radio emissions Recent observations and analyses of heliospheric 2-3 kHz radio emissions

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...51g&link_type=abstract

Iowa Univ., International Solar Wind 8 Conference, p. 51

Computer Science

Radio Emission, Plasma Density, Heliosphere, Very Low Frequencies, Voyager 1 Spacecraft, Solar Wind, Boundaries, Voyager 2 Spacecraft

Scientific paper

Since the discovery of the 2-3 kHz heliospheric radio emissions in the Voyager data over twelve years ago, there have been two major events, the first in 1983-84 and the second in 1992-93, as well as several minor events. Strong evidence now exists that these radio emissions are generated by interactions that take place in the outer regions of the heliosphere, most likely in response to strong interplanetary shocks and associated disturbances propagating outward from the Sun. Just where these interactions take place is still a subject of controversy. The three main possibilities are at or near the termination shock, between the termination shock and the heliopause and at or near the heliopause. In this paper we will review the present state of knowledge concerning the 2-3 kHz radio emissions, including the most recent data from Voyagers 1 and 2. These observations will then be compared to models that have been proposed to explain the origin of the radio emissions. Depending on the model, various estimates can be made concerning the plasma densities in the region where the radio emission is produced, and the distance to the source. The constraints provided by these models on the size and structure of the heliosphere are discussed.

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