The Jovian left hand polarized radiation

Details The Jovian left hand polarized radiation The Jovian left hand polarized radiation

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...276..603l&link_type=abstract

Astronomy and Astrophysics, Vol. 276, p. 603 (1993)

Astronomy and Astrophysics

Astrophysics

5

Planets Individual: Jupiter - Radio Emission: Solar System

Scientific paper

Very few studies have been made of Jupiter's left-hand polarized (LH) emission. Here we investigate in detail the LH emission from 2.8 MHz to 40 MHz by analysing the Voyager Planetary Radio Experiment (PRA) data during the two months when the spacecraft were close to Jupiter. We consider separately the observations by Voyager 1 and Voyager 2, before and after closest approach, in order to study the longitudinal and latitudinal beaming, and search for any local time effect.
The average statistical properties of the LH radiation are contrasted to the RH one which is better known. The main findings can be summarized as follows: 1) The occurrence probability of the RH emission is about the same as the LH at frequencies less than 5 MHz, and a maximum of probability is found at about 8 MHz. 2) At frequencies above 15 MHz the LH probability decreases dramatically. 3) The probability spectra in CML of both RH and LH show a continuity from low to high frequencies. 4) In the low frequency range, below about 10 MHz, the occurrence patterns are very simple and the RH pattern is complementary to the LH one: RH radiation occurs mainly from 150° to 300° CML, and LH radiation from 310° to 110°. 5) At higher frequencies the two patterns become complex. 6) The probability spectra in to phase show that the to-related peaks exist in both RH and LH emission at 90-120° and at 240-300°, and that they extend to the lowest frequency, 2.5 MHz. 7) The latitude effect is mainly significant for the RH emission where it modifies the shape of the main peaks. 8) The local time affects the probability spectrum: the probability drops significantly after closest approach for both RH and LH emission.
We interpret these results in terms of beaming of the radiation in hollow cones, i.e. on the surface of conical sheets of large opening angle, 50° to 80°. For the emission at f ≲ 10 MHz, these conical sheets are in polar regions, L ≍ 6 to 10, at R ≳ 1.4 Rβ where the field is more dipolar than at lower altitudes (and higher frequencies), and they are active at all longitudes. An observer near the plane of the ecliptic in the hemisphere centered on longitude 200° (20°) is located along the surface of at least one of the cones of the northern (southern) auroral zone and receives RH (LH) radiation. For the to-related radiation at higher frequencies, ≳ 20 MHz, the situation is similar except that conical sheets are activated by to in only a small range of longitudes.

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