Sounding the flanks of the Earth's bow shock to <formula>-230RE: ISEE 3 observations of terrestrial radio sources down to 1.3 times the solar wind plasma frequency

Details Sounding the flanks of the Earth's bow shock to <formula>-230RE: ISEE 3 observations of terrestrial radio sources down to 1.3 times the solar wind plasma frequency Sounding the flanks of the Earth's bow shock to <formula>-230RE: ISEE 3 observations of terrestrial radio sources down to 1.3 times the solar wind plasma frequency

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jgr...10323565s&link_type=abstract

Journal of Geophysical Research, Volume 103, Issue A10, p. 23565-23580

Physics

3

Interplanetary Physics: Planetary Bow Shocks, Interplanetary Physics: Solar Wind Plasma, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Radio Science: Instruments And Techniques

Scientific paper

We sound the Earth's bow shock and magnetosheath to X(GSE)~=-230RE by analyzing the propagation of low-frequency terrestrial radio emissions through these regions to ISEE 3 in the interplanetary (IP) medium in the 0300-0400 LT sector less than 200RE from Earth. Two sources are seen tailward of the Earth's direction, the farther the lower the frequency and sometimes away from the shock: the spike of low-frequency (LF) bursts from 1.3 to 2fp.sw (fp.sw is the solar wind plasma frequency) and the auroral kilometric radiation (AKR) above 2fp.sw. IP scattering can help explaining how radiation can reach the spacecraft while traveling sunward from X~=-230RE; but only if the whole of the apparent source on the shock flank is far enough tailward. The minimum frequency at which the spike can be located is in most cases within 10% of the maximum plasma frequency fmax.sh across the shock calculated from the Rankine-Hugoniot equations. Models of the bow shock-magnetosheath density distribution (fmax.sh(X)) are thus built so that the LF radiation becomes occulted for X~2fp.sw which appears closer to Earth than the burst spike. This probably implies that the auroral and the LF burst spike radiations cross the shock at about the same time but at different places.

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