Low Frequency (<1 MHz) Solar Radio Burst Occurrence as a Measure of Solar Activity: Ulysses Observations from 1993 to 2002

Details Low Frequency (<1 MHz) Solar Radio Burst Occurrence as a Measure of Solar Activity: Ulysses Observations from 1993 to 2002 Low Frequency (<1 MHz) Solar Radio Burst Occurrence as a Measure of Solar Activity: Ulysses Observations from 1993 to 2002

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh41a..04m&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH41A-04

Astronomy and Astrophysics

Astronomy

6954 Radio Astronomy, 7534 Radio Emissions, 2118 Energetic Particles, Solar

Scientific paper

At frequencies less than 1 MHz, there are only two common varieties of solar radio bursts - type II bursts, excited by shock-accelerated electrons, and type III bursts, excited by suprathermal electrons from solar flares. Type III bursts are two orders of magnitude more common than type II bursts at these frequencies. Because the type III bursts are indirectly caused by solar flares, their occurrence probability tracks other measures of solar activity, such as sunspot number, quite well. Because the low frequency extents of type III bursts result when electrons depart the corona on open field lines, these bursts may relate to the ability of other energetic particles to escape from the corona. In this presentation, Ulysses observations of type III burst occurrence at a number of frequencies are correlated with various measures of solar activity. Comparisons with SEP event occurrence will be discussed.

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