Acknowledgments

 

The Star Scanner science would not be possible without the work of hundreds of people including the original designers, test engineers, the Galileo Flight Team and management, as well as scientists and engineers across JPL. The author would especially like to thank Shadan Ardalan for endless hours of scheming how to better operate the Star Scanner as well as Project Managers Eilene Theilig, Claudia Alexander and Jim Erickson for tolerating and funding the work required to make the Star Scanner do more than its designers thought possible.

 

The picture of Jupiter and Io on the Engineering and Design page and the two figures on the Amalthea page were drawn by the program SOAP from The Aerospace Corp.

 

Much of this scientific work referred to in this web site was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This web page is the personal work of the Principal Investigator and does not necessarily constitute or imply endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology.

 

 

References

 

[1] Van Allen, J.A. “High Energy Particles in the Jovian Magnetosphere.” Jupiter: Studies of the Interior, Magnetosphere and Satellites, Univ. of Arizona Press, 1976.

 

[2] Fillius, W.  “The Trapped Radiation Belts of Jupiter.”  Jupiter: Studies of the Interior, Magnetosphere and Satellites, Univ. of Arizona Press, 1976.

 

[3] Divine N., Garrett H.B., “Charged particle distributions in Jupiter’s magnetosphere,” J. Geo. Res. 88(A9), pp. 6889-6903, Sept. 1983.

 

[4]  Bolton S.J., et al., “Ultra-relativistic electrons in Jupiter's radiation belts,” Nature, 415 (6875): 987-991 Feb 28 2002.

 

[5] Williams D.J., et al., “Electron beams and ion composition measured at Io and in its torus”,  Science,  274 (5286): 401-403 Oct 18, 1996.

 

[6]  Yu Z.J., et al. “The time variability of the Io torus,” Fall AGU, Eos. Trans. AGU, 80(46), Fall Meeting Suppl. 1999.

 

[7]  Otero S., Fieseler P.D., Lloyd, C.,” Delta Velorum is an Eclipsing Binary,” Commissions 27 and 42 of the IAU Information Bulletin on Variable Stars, Number 4999,  Dec 7, 2000: see http://www.konkoly.hu/cgi-bin/IBVS?4999

 

[8] AAVSO Eclipsing Binary update Web Page: see http://www.aavso.org/committees/eb/ebupdate11.stm

 

[9]  Otero S., Fraser B., Lloyd, C “The Optical Behaviour of delta Scorpii,” Commissions 27 and 42 of the IAU Information Bulletin on Variable Stars, Number 5026,  Jan 29, 2001: see http://www.konkoly.hu/cgi-bin/IBVS?5026

 

[10]  Gandet T.L, Otero S., Fraser B., West D.J.,” delta Scorpii: Visual Photometric Variability in 2000-2002,” Commissions 27 and 42 of the IAU Information Bulletin on Variable Stars, Number 5352,  Dec 13, 2002: see http://www.konkoly.hu/cgi-bin/IBVS?5352

 

[11]  Evans, R. “Galileo Millenium Mission Radiation Dose”, Inter-office Memorandum 5052-2000-103, June 8, 2000.

 

[12]  Fieseler P.D.,  Ardalan S.M., Frederickson A.R., “The Radiation Effects on Galileo Spacecraft Systems at Jupiter,” IEEE Transactions on Nuclear Science, Dec 2002.

 

[13]  Summary of Known Volcanic Activity, Early 1995 – Present - Web Page: See http://physics.uwyo.edu/~rhowell/io_1999.htm

 

[14]  Fieseler P.D., “The Galileo Star Scanner as an Instrument for Measuring Energetic Electrons in the Jovian Environment,” Master’s thesis, Univ. of Southern California, Dec. 2000.

 

[15] Russell C.T., Fieseler P.D., Bindschadler D., Yu Z.J., Joy S.P., Khurana K.K. and Kivelson M.G., “Large scale changes in the highly energetic charged particles in the region of the Io torus,” Advances in Space Research, Vol 28, No 10, pp. 1495-1500, 2001.

 

[16] Russell C.T., Georgilas S., Mauk  B.H., and Williams D.J., “Io as the Source of Disturbances in the Inner Jovian Magnetosphere”, EGS General Assembly, Nice, France, April 2002.

 

[17] Mauk B.H., Williams, D.J., “Understanding Io’s Space Environment Interaction: Recent Energetic Electron Measurements from Galileo”, Journal of Geophysical Research, Vol 106, no A11, pp 26,195 – 26,208, Nov 1, 2001.

 

[18] Ratliff J.M., Fieseler P.D., Jun I and Garrett, H.B., “Estimate of Jovian High-energy Electron Flux at Range R > 2 RJ, Using Data from the Galileo Spacecraft’s Final Full Orbit”, EGS-AGU-EUG Joint Conference, Apr 7-11 2003, Nice France.

 

[19] Birnbaum M.M., R.L. Bunker, and J.T. Tavolacci. “A Radiation-hardened Star Scanner for Spacecraft Guidance and Control”. Journal of Guidance, Control and Dynamics, vol 6, no. 1, pp. 39-46. 1983.

 

[20] Armstrong, T, Miller S., Wadley S., McEntire R., Williams D., “Results from the Galileo Energetic Particle Detector During the Amalthea Encounter of November 5th, 2002”, Poster presentation at AGU, Dec 9, 2003, SM22B-0255. Also at http://galileo.ftecs.com/Amalthea/html/index_122603_1523.html

 

[21] Fieseler, P.D. et al., “The Galileo Star Scanner Observations at Amalthea” Icarus, vol 169, no 2, 2004.

 

 

 

 

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