High-energy charged particles in the innermost jovian magnetosphere

Science

Volumn 272, Issue 5263, 1996, Pages 856-858

  Fischer, H M ^a   Pehlke, E ^a   Wibberenz, G ^a   Lanzerotti, L J ^b   Mihalov, J D ^c  

^a UNIVERSITY OF KIEL   (Germany)

^b LUCENT TECHNOLOGIES   (United States)

^c NASA AMES RESEARCH CENTER   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0001125640     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.272.5263.856     Document Type: Article

References (18)

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3. Special issue on Pioneer 10, Science 183 (1974); special issue on Pioneer 10, J. Geophys. Res.79 (1974).
4. -2, form the rear shielding of the telescope. A number of instrument performance effects during flight - such as acceptance curves for energy channels, final geometrical factors, deadtime losses, stray coincidences, and multiparticle events, as well as the influence of the heat shield - are accounted for here only with initial estimates. The instrument temperature during the encounter was <0°C, so no thermal noise problems existed in the detectors.
5. For the E1, E2, and E3 electron thresholds in Table 1, the tabulated values are obtained from range-energy relations. When the scattering of incident electrons from the aft heat shield is considered, the median energies detected by these thresholds, based on Monte Carlo transport calculations, correspond to higher energies that depend on the energy spectrum of the incident electrons. The E2, P2, P3, He, and HV measurements use coincidence detections between the two solid-state detectors.
6. L. J. Lanzerotti et al., Science 272, 858 (1996).
7. 2 sr for (E1 and P1) and (E2, P2, P3, He, and HV), respectively.
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18. We thank the NASA Ames Galileo Project Office, B. Chin, A. Wilhelmi, C. Sobeck, M. Smith, R. Young, and the technical staff for assistance during the long interval of excellent cooperation. We are grateful to F. Gliem and J. Bach (University of Braunschweig); F. Wendler, P. Glasow, and G. Eberlein (Siemens Company, Erlangen, Germany); the technical staff of the Dornier-System Company (Friedrichshafen, Germany); and the technical and administrative staff of VARTA Battery Company (Kelkheim and Hannover, Germany) for their help in making the LRD-EPI instrument a success. Thanks are due to E. Böhm (University of Kiel) for his contributions in scientific discussions and his assistance in data evaluation and with programs for particle track simulations in the detector telescope; S. Sievers (University of Kiel) for his help with the figures; and J. A. Van Allen (University of Iowa) for helpful suggestions. The EPI investigations were supported by the German Agency tor Space Activities DARA by grant number 50 QJ 9001 7.