Solar Wind Magnetic Field Bending of Jovian Dust Trajectories-Reference-Cited by-同舟云学术

Solar Wind Magnetic Field Bending of Jovian Dust Trajectories

Published:1996-11-29 Issue:5292 Volume:274 Page:1501-1503
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Zook H. A.¹,Grün E.²,Baguhl M.²,Hamilton D. P.³,Linkert G.²,Liou J.-C.¹,Forsyth R.⁴,Phillips J. L.⁵

Affiliation:

1. H. A. Zook and J.-C. Liou, SN3, NASA Johnson Space Center, Houston, TX 77058, USA.

2. E. Grün, M. Baguhl, G. Linkert, Max-Planck-Institut für Kernphysik, Postfach 103980, 69029 Heidelberg, Germany.

3. D. P. Hamilton, Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA.

4. R. Forsyth, The Blackett Laboratory, Imperial College, London SW7 2BZ, UK.

5. J. L. Phillips, Los Alamos National Laboratory, Los Alamos, NM 87545, USA.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference18 articles.

1. Ulysses Dust Measurements Near Jupiter

2. Grün E., et al., Nature 262, 428 (1993).

3. Baguhl M., et al., Planet. Space Sci. 41, 1085 (1994).

4. ϕ m = 0 when the CDD axis points as close as possible to ecliptic north. Events of digital amplitude higher than 8 are left out of Fig. 1 as they are largely due to impacts by interstellar grains (2 3) and nearly all occur between streams. This omission highlights the stream data. With 15 impacts in a stream and considering the 140° fov of the CDD the true radiant of a monodirectional stream is known at 95% confidence to ±10°. The spacecraft spin axis is co-aligned with the high gain antenna which points toward the Earth. The central axis of the 140° fov CDD is fixed to point at 85° to the Ulysses spin axis.

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

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