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Science 27 September 1991:
Vol. 253. no. 5027, pp. 1525 - 1528
DOI: 10.1126/science.253.5027.1525
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Articles

Energetic Particles at Venus: Galileo Results

D. J. WILLIAMS 1, R. W. MCENTIRE 1, S. M. KRIMIGIS 1, E. C. ROELOF 1, S. JASKULEK 1, B. TOSSMAN 1, B. WILKEN 2, W. STÜDEMANN 2, T. P. ARMSTRONG 3, T. A. FRITZ 4, L. J. LANZEROTTI 5, and J. G. ROEDERER 6

1 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723
2 Max Planck Institute für Aeronomie, Katlenburg-Lindau, Federal Republic of Germany
3 University of Kansas, Lawrence, KS 66044
4 Los Alamos National Laboratory, Los Alamos, NM 87545
5 AT&T Bell Laboratories, Murray Hill, NJ 07974
6 University of Alaska, Fairbanks, AK 99775

At Venus the Energetic Particles Detector (EPD) on the Galileo spacecraft measured the differential energy spectra and angular distributions of ions >22 kiloelectron volts (keV) and electrons > 15 keV in energy. The only time particles were observed by EPD was in a series of episodic events [0546 to 0638 universal time (UT)] near closest approach (0559:03 UT). Angular distributions were highly anisotropic, ordered by the magnetic field, and showed ions arriving from the hemisphere containing Venus and its bow shock. The spectra showed a power law form with intensities observed into the 120- to 280-keV range. Comparisons with model bow shock calculations show that these energetic ions are associated with the venusian foreshock-bow shock region. Shock-drift acceleration in the venusian bow shock seems the most likely process responsible for the observed ions.

Revised on April 26, 1991
Accepted on July 1, 1991


THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Magnetic Field Studies of the Solar Wind Interaction with Venus from the Galileo Flyby.
M. G. KIVELSON, C. F. KENNEL, R. L. MCPHERRON, C. T. RUSSELL, D. J. SOUTHWOOD, R. J. WALKER, C. M. HAMMOND, K. K. KHURANA, R. J. STRANGEWAY, and P. J. COLEMAN (1991)
Science 253, 1518-1522
   Abstract »    PDF »
Plasma Observations at Venus with Galileo.
L. A. FRANK, W. R. PATERSON, K. L. ACKERSON, F. V. CORONITI, and V. M. VASYLIUNAS (1991)
Science 253, 1528-1531
   Abstract »    PDF »


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