Additional Information from Week 1 and Readings for Week 2
  1. Textbooks for the class are "Satellites", (1986), J. Burns and M. Matthews, ed., Univ. of Arizona Press ('required') and "Satellites of the Outer Planets: Worlds in their Own Right", D. Rothery, 2nd edition, (1992) (recommended). Both of these are available from the Brown Bookstore.
  2. Notes from the Introduction:
    1. What is the role of tidal heating in compositional evolution of Io?
    2. What is the real composition of Io?
    3. What is the relation to the external environment?
    4. What is the nature of the crust?
    5. What is the driving force for volcanism?
    6. How can one distinguish the energy derived from tidal heating from that associated with the general thermal evolution?
    7. Where is the ancient crust of Io?

    1. What is the surface and subsurface composition?
    2. What is the proportion of silicates and water?
    3. Is there a liquid asthenosphere?
    4. What is the origin of the fracutre systems?
    5. What processes are responsible for the surface evolution and the albedo?
    6. What is the nature and evolution of the crust and the relationship of water and silicates?

    1. What is the nature of the dark and bright terrains?
    2. What are the realtive and absolute age relationships between these?
    3. What is the origin(s) of ridges and grooves?
    4. What is the composition and rheology of the crust with time?
    5. Why palimpsests?

    1. Palimpsests and ringed structures: Are they impacts or negative diapirs?
    2. What is the nature of the dark terrain?
    3. What makes ejecta bright?
    4. What is the relation of surface geological features to activity in the interior?
    5. Why is the central part of Valhalla bright? Impact melt or volcanism?

    Ganymede and Callisto Comparison: Why are they so similar yet so different?

  3. General Assignments:
    On the basis of the input from you last week, the following assignments have been made. I think it pretty much represents everyone's priorities at least in a general way. The key is IA = Irene Antonenko, AY = Aileen Yingst, LP = Louise Prockter, CW = Cathy Weitz, MG = Marty Gilmore, GC = Geoff Collins, LL = Lin Li, SH = Steve Herzog. I will assign specific readings the week before the class. For the ones for this Wednesday, see later in this memo. Each person has six assignments to report on.

    1. (February 14th): Satellite accretion; structure, properties and chemistry of ices. (IA, MG, SH, AY)
    2. (February 16th): Orbital evolution and tidal heating. (IA, LP, GC, LP)
    3. (February 19th): Satellite thermal evolution and interior processes. (CW, AY, MG, SH)
    4. (February 21st): Io: Geology, volcanic processes and evolution. (AY, LP, CW, MG)
    5. (February 28th): Impact cratering on icy satellites: Processes. (GC, IA, LL, CW)
    6. (March 6th): Impact cratering on icy satellites: History. (GC, LL, MG, IA)
    7. (March 13th): Ganymede and Callisto: Formation and evolution of dark terrain. (LP, MG, SH, LL)
    8. (April 3rd): Ganymede: Ice volcanism and emplacement of bright terrain. (IA, LP, CW, GC).
    9. (April 10th): Ganymede: Grooved terrain characteristics, formation and evolution. (LP, GC, MG, LL)
    10. (April 17th): Europa: Resurfacing, band formation and tidal stresses. (GC, SH, LL, AY)
    11. (April 24th): Europa: Geological evolution, surface and interior structure. (SH, CW, LL, AY)
    12. (May 1st): Galilean Satellites: Surface composition, regolith processes, and exterior processes. (CW, SH, IA, AY).

  4. Reading Assignments for Wednesday, February 14th Class (Satellite Accretion; structure, properties, and chemistry of ices): Starred items are the most significant to read for people not responsible for presentations. Presenters should at least scan and incorporate important aspects of the non-starred items. Presentations should be about 20 minutes with about 10 minutes for discussion.

      Aileen Yingst
      • Lewis, J.S., Low temperature condensation from the solar nebula, Icarus, 16, 241-252, 1972.
      • *Stevenson, D. J. et al., Origins of Satellites, Satellites, Chapter 2, 39-88.

      • *Whalley, E., The physics of ice: Some fundamentals of planetary glaciology, in Ices in the Solar System (J. Klinger et al., eds.), Reidel, 9-37, 1985.

      Steve Herzog:
      High-pressure ice phases:

      • *Poirier, J. P., Rheology of ices: a key to the tectonics of the ice moons of Jupiter and Saturn, Nature, 299, 683-688, 1982.
      • Poirier, J.P., et al., Viscosity of high-pressure ice VI and evolution and dynamics of Ganymede, Nature, 292, 225-227, 1981.

      Irene Antonenko:
      Rheology of cold water ice:

      • *Durham, W.B., et al., Experimental deformation of polycrystalline H2O ice at high pressure and low temperature: Preliminary results, Proc. LPSC 14th in JGR, 88, B377-B392, 1983.

      Rheology of water ice + silicates:

      • Durham, W.B., et al., Effects of dispersed particulates on the rheology of water ice at planetary conditions, JGR, 97, 20883-20897.

      Marty Gilmore:
      Properties of ammonia-water mixtures:

      • *Kargel, J.S., et al., Rheological properties of ammonia-water liquids and crystal-liquid slurries: Planetological applications, Icarus, 89, 93-112, 1991.

      Clathrate hydrates:

      • Miller, S.L., Clathrate hydrates in the solar system, in Ices in the Solar System (J. Klinger et al., eds.), Reidel, 59-79, 1985.