Computer Science – Sound
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984georl..11..267c&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 11, March 1984, p. 267-270.
Computer Science
Sound
38
Ionospheric Sounding, Magnetic Measurement, Planetary Ionospheres, Planetary Magnetic Fields, Venus Atmosphere, Flow Velocity, Magnetic Flux, Pioneer Venus 1 Spacecraft, Venus, Ionosphere, Magnetic Fields, Evolution, Magnetometer, Pvo, Pioneer Venus, Orbiters, Solar Wind, Pressure, Time Scale, Shape, Convection, Flux, Plasmas, Diffusion, Decay, Structure
Scientific paper
Large-scale magnetic fields are often observed in the ionosphere of Venus by the magnetometer on the Pioneer Venus Orbiter, especially near the subsolar point or when the solar wind dynamic pressure is high. An equation for the time evolution of the magnetic field is derived which includes both a term representing the time rate of change of the field due to the convection of magnetic flux by plasma motions, and a magnetic diffusion/dissipation term. The ionospheric plasma velocities required by these equations were obtained by numerically solving the momentum equation. Numerical solutions to the magnetic field equation indicate that large-scale magnetic fields, which are not being actively maintained, decay with time scales ranging from tens of minutes to several hours. The vertical convection of magnetic flux enables magnetic field structures deep within the ionosphere to persist longer than would otherwise be expected. This vertical convection also explains the shape of these structures.
Cravens Thomas E.
Nagy Andrew F.
Shinagawa Hiroyuki
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