Magnetic field draping enhancement at Venus: Evidence for a magnetic pileup boundary

Details Magnetic field draping enhancement at Venus: Evidence for a magnetic pileup boundary Magnetic field draping enhancement at Venus: Evidence for a magnetic pileup boundary

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003georl..30qssc1b&link_type=abstract

Geophysical Research Letters, Volume 30, Issue 17, pp. SSC 1-1, CiteID 1876, DOI 10.1029/2003GL017271

Physics

6

Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies, Magnetospheric Physics: Planetary Magnetospheres (5443, 5737, 6030), Planetology: Solar System Objects: Venus

Scientific paper

The absence of a global-scale dynamo-generated magnetic field and the existence of an ionosphere at Venus and Mars caused many to predict that their solar wind interaction would be similar. After Pioneer Venus Orbiter (PVO) observations, it was concluded that the global aspects of the Venusian interaction could be well described by single-fluid models. According to these models, the magnetic field draping should develop progressively from the shock down to the ionopause. A recent study at Mars, where a ``Venus-like'' interaction was expected, showed that draping is prominent only inside the magnetic pileup boundary (MPB), a well-defined plasma boundary located between the shock and the ionopause first reported at comets, but never at Venus. From an identical analysis on PVO magnetometer data, we report a dramatic enhancement of draping on the dayside of Venus. Then, we deduce the existence of a Venusian counterpart of the Martian and cometary MPB.

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