Type III radio bursts observed by ULYSSES pole to pole, and simultaneously by wind.

Details Type III radio bursts observed by ULYSSES pole to pole, and simultaneously by wind. Type III radio bursts observed by ULYSSES pole to pole, and simultaneously by wind.

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...316..406l&link_type=abstract

Astronomy and Astrophysics, v.316, p.406-412

Astronomy and Astrophysics

Astrophysics

6

Sun: Radio Radiation, Activity, Corona

Scientific paper

We consider 555 type III bursts observed by Ulysses and/or Wind while Ulysses traversed a large range of longitude and latitude. We find: 1) The percentage of bursts seen by both spacecraft was 59.5%. It was higher, about 80%, when Ulysses was to the south and east of the Sun as seen from Wind. It decreased to about 50% when Ulysses was near the ecliptic behind the Sun, and it remained near 50% as Ulysses moved to the north and west. 2) The distribution of low frequency cutoffs f_lo_ of type III radiation is very similar for bursts seen by Ulysses and those seen by Wind, whereas the distribution of the in-situ plasma frequency f_p_ at the two spacecraft is very different. Many bursts descend to close to f_p_~30kHz at Wind but few descend to the lower f_p_~10kHz at Ulysses. We confirm earlier findings that f_lo_ is rarely lower than about 20kHz. 3) Statistically, the low frequency limit depends strongly on the burst intensity, being about four times lower for strong bursts than for weak bursts. We consider three hypotheses for the close relation between intensity and f_lo_: proximity of the burst source to one spacecraft or the other, directivity and propagation effects, and density and speed of the fast electron stream. We conclude that, while the first two may be important for some bursts, for many others the character of the electron stream is the dominant factor in establishing both the burst intensity and the lowest frequency attained.

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