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The Abundant Irregular Satellites of the Giant Planets

Published online by Cambridge University Press:  30 March 2016

Scott S. Sheppard  and
David C. Jewitt
Scott S. Sheppard
Affiliation:
Univ. of Hawaii, Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, Hi 96822, USA
David C. Jewitt
Affiliation:
Univ. of Hawaii, Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, Hi 96822, USA

Abstract

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Irregular satellites have eccentric orbits that can be highly inclined or even retrograde relative to the equatorial planes of their planets. These objects cannot have formed by circumplanetary accretion as did the regular satellites which follow un-inclined, nearly circular, pro-grade orbits. Instead, they are likely products of early capture from heliocentric orbit. The study of the irregular satellites provides a unique window on processes operating in the young solar system. Recent discoveries around Jupiter (45 new satellites), Saturn (13), Uranus (9), and Neptune (5) have almost increased the number of known irregular satellites by a factor of ten and suggest that the gas and ice giant planets all have fairly similar irregular satellite systems. Dynamical groupings were most likely produced by collisional shattering of precursor objects after capture by their planets. Jupiter is considered as a case of special interest. Its proximity allows us to probe the fainter, smaller irregular satellites to obtain large population statistics in order to address the questions of planet formation and capture.

Type
II. Special Scientific Sessions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 898 - 900
Copyright
Copyright © Astronomical Society of Pacific 2005

References

Carruba, V. et al. 2002, Icarus, 158, 434 Google Scholar
Colombo, G. & Franklin, F. 1971, Icarus, 15, 186 Google Scholar
Gladman, B. et al. 2000, Icarus, 147, 320 Google Scholar
Gladman, B. et al. 2001, Nature, 412, 163 Google Scholar
Heppenheimer, T. & Porco, C. 1977, Icarus, 30, 385 CrossRefGoogle Scholar
Holman, M. et al. 2003, IAU Circ., 8047 Google Scholar
Jewitt, D., Sheppard, S., & Porco, C. in press, in Jupiter II, ed. Bagenal, F., Cambridge University Press, Cambridge, p. 236 Google Scholar
Nesvorny, et al. 2003, AJ, 126, 398 Google Scholar
Pollack, J., Burns, J. & Tauber, M. 1979, Icarus, 37, 587 Google Scholar
Sheppard, S. & Jewitt, D. 2003, Nature, 423, 261 Google Scholar
Sheppard, S. et al. 2003, IAU Circ, 8193 Google Scholar