Distribution of Rock, Metals, and Ices in Callisto-Reference-Cited by-同舟云学术

Distribution of Rock, Metals, and Ices in Callisto

Published:1998-06-05 Issue:5369 Volume:280 Page:1573-1576
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Anderson J. D.¹²,Schubert G.¹²,Jacobson R. A.¹²,Lau E. L.¹²,Moore W. B.¹²,Sjogren W. L.¹²

Affiliation:

1. J. D. Anderson, R. A. Jacobson, E. L. Lau, W. L. Sjogren, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109–8099, USA.

2. G. Schubert and W. B. Moore, Department of Earth and Space Sciences, Institute of Geophysics and Planetary Physics, University of California Los Angeles, California 90095–1567, USA.

Abstract

Radio Doppler data from a single encounter (C3) of the Galileo spacecraft with Callisto, the outermost Galilean moon of Jupiter, indicated that Callisto was probably undifferentiated. Now, similar data from a second encounter (C9) corroborate this conclusion, but more accurate data from a third encounter (C10) indicate that the rock and ice within Callisto have partially, but not completely, separated. Callisto may be differentiated into a rock-metal core less than 25 percent of Callisto's radius, an outer layer of clean ice less than 350 km thick, and a middle layer of mixed rock and ice. Models in which ice and rock are mixed all the way to the center of Callisto are also consistent with the data.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference24 articles.

1. The first encounter (C3) occurred on 4 November 1996 at 11:47:09 the second (C9) occurred on 25 June 1997 at 13:47:50 and the third (C10) occurred on 17 September 1997 at 00:18:55 where the encounter times are expressed in Universal Time Coordinated (UTC) at the spacecraft and the encounter designation Cn refers to an encounter with Callisto on the spacecraft's n th orbital revolution of Jupiter.

2. See for example T. D. Moyer Tech. Rep. No. TR 32-1527 (Jet Propulsion Laboratory Pasadena CA 1971)

3. B. D. Tapley in Recent Advances in Dynamical Astronomy B. D. Tapley and V. Szebehely Eds. (Reidel Dordrecht Netherlands and Boston MA 1973) pp. 396-425

4. J. D. Anderson in Experimental Gravitation B. Bertotti Ed. (Academic Press New York 1974) pp. 163-199.

5. W. M. Kaula Theory of Satellite Geodesy (Blaisdell Waltham MA 1966). The expression for V is V(r φ λ)=GMr 1+∑n=2∞ ∑m=0n Rrn×(Cnm cos mλ+Snm sin mλ)Pnm(sinφ) where M is the satellite's mass and G is the gravitational constant G = 6.6728 ± 0.0016 × 10 −11 m 3 kg −1 s −2 [see E. R. Cohen and B. N. Taylor Phys. Today 49 BG9 (1996)]. The spherical coordinates ( r φ λ) are referred to the center of mass with r the radial distance φ the latitude and λ the longitude on the equator. Callisto's reference radius R is 2403 km [see M. E. Davies et al. Celes. Mech. 53 377 (1992)]. P nm is the associated Legendre polynomial of degree n and order m and C nm and S nm are the corresponding coefficients determined from the data.

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