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Effect of Enceladus's rapid synchronous spin on interpretation of Cassini gravity

Mckinnon, William B.

Geophysical Research Letters, 16 April 2015, Vol.42(7), pp.2137-2143 [Periódico revisado por pares]

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  • Título:
    Effect of Enceladus's rapid synchronous spin on interpretation of Cassini gravity
  • Autor: Mckinnon, William B.
  • Assuntos: Icy Satellite ; Cassini Mission ; Gravity Model ; Enceladus Ocean
  • É parte de: Geophysical Research Letters, 16 April 2015, Vol.42(7), pp.2137-2143
  • Descrição: Enceladus's degree 2 gravity, determined by Cassini, is nominally nonhydrostatic to 3σ (/ = 3.38–3.63, as opposed to 10/3). Iess et al. (2014) interpret this in terms of a hydrostatic interior (core) and isostatic (not hydrostatic) floating ice shell. Enceladus's rapid (1.37 d) synchronous spin and tide distorts its shape substantially, though, enough that the predicted hydrostatic / is not 10/3 but closer to 3.25. This leads to the following revision to the internal picture of Enceladus, compared with Iess et al.: (1) the satellite's core is somewhat smaller and slightly denser (190 km radius and 2450 kg/m); (2) the compensation depth (shell thickness) of the global (degree 2) ice shell is ≈ 50 km, rather close to the base of the modeled ice + water layer; and (3) the compensation depth (shell thickness) beneath the South Polar Terrain (from ) remains shallower (thinner) at ≈ 30 km, independent of but influenced by the degree 2 solution. Enceladus' rapid spin requires higher‐order theory for degree 2 gravity and shape Cassini gravity and shape imply a global ocean nearly but not completely frozen Ice shell much thinner over the South Polar Terrain facilitating plume venting

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