Dust Measurements During Galileo's Approach to Jupiter and Io Encounter-Reference-Cited by-同舟云学术

Dust Measurements During Galileo's Approach to Jupiter and Io Encounter

Published:1996-10-18 Issue:5286 Volume:274 Page:399-401
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Grün E.¹,Hamilton D. P.²,Riemann R.¹,Dermott S.³,Fechtig H.¹,Gustafson B. A.³,Hanner M. S.⁴,Heck A.¹,Horanyi M.⁵,Kissel J.¹,Krüger H.¹,Lindblad B. A.⁶,Linkert D.¹,Linkert G.¹,Mann I.⁷,McDonnell J A. M.⁸,Morfill G. E.⁹,Polanskey C.⁴,Schwehm G.¹⁰,Srama R.¹,Zook H. A.¹¹

Affiliation:

1. E. Grün, H. Fechtig, A. Heck, J. Kissel, H. Krüger, D. Linkert, G. Linkert, R. Riemann, R. Srama, Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany.

2. D. P. Hamilton, University of Maryland, College Park, MD 20742-2421, USA.

3. S. Dermott and B. A. Gustafson, University of Florida, Gainesville, FL 32611, USA.

4. M. S. Hanner and C. Polanskey, Jet Propulsion Laboratory, Pasadena, CA 91109, USA.

5. M. Horanyi, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309, USA.

6. B. A. Lindblad, Lund Observatory, 221, Lund, Sweden.

7. I. Mann, Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany.

8. J. A. M. McDonnell, University of Kent, Canterbury, CT2 7NR, UK.

9. G. E. Morfill, Max-Planck-Institut für Extraterrestrische Physik, 85740 Garching, Germany.

10. G. Schwehm, European Space Research and Technology Centre, 2200 AG Noordwijk, Netherlands.

11. H. A. Zook, NASA Johnson Space Center, Houston, TX 77058, USA.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference13 articles.

1. Grün E., et al., Space Sci. Rev. 60, 317 (1992). The Galileo dust detector had a sensitive area of 0.1 m2 and a 140°-wide conical FOV. It was mounted on the spinning section of the Galileo spacecraft at an angle of 55° with respect to the positive spin axis (opposite to the antenna direction which pointed toward Earth). Only dust particles with relative velocity vectors within the FOV of the detector could be measured. The impact direction was determined by the spin position (or rotation angle) of the spacecraft at the time of impact. This sensor mounting direction constrained the directions from which dust grains could be sensed. This limitation varied with spacecraft rotation angle and with spacecraft location along its trajectory. During Galileo's approach to Jupiter dust particles impacting the DDS from the inner jovian system (that is, from inside the position of Galileo) could be detected when the detector was facing Jupiter; at a spin position half a rotation later DDS was facing away from Jupiter and these particles could not enter the detector. Shortly after Galileo's CA to Jupiter, Jupiter and the inner jovian system was in the Earth-facing hemisphere as seen from Galileo, and no dust grains emanating from that region could reach the dust detector

2. Grün E., et al., Astron. Astrophys. Suppl. 92, 411 (1992).

3. Ulysses Dust Measurements Near Jupiter

4. Grün E., et al., Nature 362, 428 (1993).

5. Grün E., et al., ibid. 381, 395 (1996).

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