Solar wind control of Jovian auroral emissions

Details Solar wind control of Jovian auroral emissions Solar wind control of Jovian auroral emissions

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11009221g&link_type=abstract

Journal of Geophysical Research, Volume 110, Issue A9, CiteID A09221

Astronomy and Astrophysics

Astronomy

2

Planetary Sciences: Solar System Objects: Jupiter, Radio Science: Radio Astronomy, Radio Science: Remote Sensing, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Energetic Particles: Precipitating

Scientific paper

The combination of Galileo/PWS and Wind/WAVES observations allows the study of the flux density variation of the Jovian hectometric emissions (HOM) observed from 31 August 1996 until 24 October 1996. It is found that the HOM emission presents periodic features; each one is called a ``HOM event.'' Such episodic emissions were concurrently observed by both experiments with similar spectral characteristics. The fluctuations of the Jovian hectometric emissions and the solar wind parameters are found to exhibit quasi-similar variations when a time lag of about 153 days is taken into consideration. Also, ``HOM enhancements,'' like the ``injection events'' first reported by Mauk et al. (1997), are found to occur at some specific longitudes. The occurrence of these magnetospheric events increases at two ``active longitudes,'' i.e., 45° CML and 180° CML. The solar wind seems to be at the origin of both phenomena. Solar particles go through the polar regions where they interact with the Jovian magnetic field and give rise in the auroral and equatorial regions to an increase of Jovian hectometric emissions and/or injection events.

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