Jupiter's magnetic field as revealed by the synchrotron radiation belts. II. Change of the 2-D brightness distribution with D_E

Details Jupiter's magnetic field as revealed by the synchrotron radiation belts. II. Change of the 2-D brightness distribution with D_E Jupiter's magnetic field as revealed by the synchrotron radiation belts. II. Change of the 2-D brightness distribution with D_E

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...347.1039d&link_type=abstract

Astronomy and Astrophysics, v.347, p.1039-1045 (1999)

Astronomy and Astrophysics

Astrophysics

6

Magnetic Fields, Plasmas, Radiation Mechanisms: Non-Thermal, Planets And Satellites: Individual: Jupiter, Radio Continuum: Solar System

Scientific paper

{We analyze the magnetic equatorial component of Jupiter's radio synchrotron radiation belts using two-dimensional images recorded by the Australia Telescope Compact Array and the Very Large Array over a period of several years, during which D_E, the Earth's declination seen from Jupiter, changed from D_E =-2.9 deg to near 0 deg. The brightness distribution of the belts changed markedly. When D_E =-2.9 deg there is a pronounced east-west asymmetry where the brightness of a region traversing the east limb is markedly different from that of the same region traversing the west limb, 180 deg of rotation later. At most longitudes lambdaIII the brightness at east limb passage is larger than at west limb passage. However, when D_E approx 0 deg, the east-west asymmetry essentially disappears. When D_E =+2.9 deg it is predicted that the east-west asymmetry will be as at -2.9 deg, but reversed. We show how these changes of appearance are simply related to D_E and the warp of Jupiter's field as described by the ``magnetic declination''. The radius, latitude and brightness of the locus of maximum intensity is determined by electrons of pitch angle alpha_eq ~ 90 deg, and its longitudinal variation depends entirely on the magnetic field of Jupiter, and not on the energy distribution of the relativistic electrons. We compare the observations with calculations from three magnetic field models and find them to be consistent in general but discrepant in detail. The differences are attributed to uncertainties in the field models, which were generated with few constraints coming from the low latitudes and small radii of the synchrotron radiation belts.

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