Tidal heating in Enceladus

By J. Meyer, J. Wisdom. 2007

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In Astronomy and Astrophysics

Citations in the corpus

The pH of Enceladus’ ocean (2015, background): “In the absence of large rates of energy input (tidal heating at Enceladus is dwarfed by solar heating at Earth; Meyer & Wisdom, 2007) and mixing, Enceladus’ ocean may equilibrate with many chemical elements in marine sediments over geologic time (apart from kinetically inhibited redox reactions of c”
New constraints on Saturn’s interior from Cassini astrometric data (2015, unknown): “In a second inversion, we assume Enceladus to be in a state of tidal equilibrium (Meyer & Wisdom, 2007), obtaining k2(I)=0.372 ± 0.003, k2(J)=0.402 ± 0.011 and k2/Q(I)=(2.07 ± 0.26) × 10-4, k2/Q(J)=(1.22 ±0.23) × 10-4.”
High heat flow from Enceladus' south polar region measured using 10–600 cm−1 Cassini/CIRS data (2011, background): “[3] It has been shown that over the long term this and other resonances are unable to produce an endogenic power greater than 1.1 GW if the dissipation factor Q of Saturn is frequency‐independent [ Meyer and Wisdom, 2007 ].”
Resonance locking as the source of rapid tidal migration in the Jupiter and Saturn moon systems (2016, background): “Studies which have assumed constant values of Q for Saturn in order to constrain the orbital evolution history (e.g., Peale et al. 1980; Meyer & Wisdom 2007, 2008; Zhang & Nimmo 2009) should be interpreted with caution.”
Accretion of Saturn's mid-sized moons during the viscous spreading of young massive rings: Solving the paradox of silicate-poor rings versus silicate-rich moons (2011, background): “341 (Gavrilov and Zharkov, 1977, see also Dermott et al., 1988; Sinclair, 1983; Meyer and Wisdom, 2007).”
Planetary habitability: lessons learned from terrestrial analogues (2014, unknown): “Reviews into how this plume might form are provided by Kieffer et al. (2006), Spencer et al. (2006); Castillo-Rogez et al. (2007); Collins & Goodman (2007); Meyer & Wisdom (2007); Nimmo et al. (2007) and McKay et al. (2008).”
Enceladus: An Active Ice World in the Saturn System (2013, background): “In the particular case that Enceladus’s eccentricity remains constant, the heat production within Enceladus is inversely proportional to Saturn’s Q and is independent of Enceladus’s k2/Q (Meyer & Wisdom 2007).”
HOW THE GEYSERS, TIDAL STRESSES, AND THERMAL EMISSION ACROSS THE SOUTH POLAR TERRAIN OF ENCELADUS ARE RELATED (2014, background): “Survival of a regional as opposed to a global body of water is also more readily reconciled with the long-term averaged tidal dissipation rate, which does not exceed 1.1 GW based on conventional estimates of Saturn’s dissipation (Meyer & Wisdom 2007).”
Tidal Dissipation in Stars and Giant Planets (2014, background): “This value is far below the lower bound quoted above, based on the migration of Mimas (and Tethys), and could help to explain the heating rate of Enceladus (cf. Meyer & Wisdom 2007).”
Tidal heating in icy satellite oceans (2014, methodology): “Homogeneous k2 k2 ¼ 3=2 _EradðWÞ _Esolid;eccðWÞ _Esolid;oblðWÞ _Esolid;eccðWÞ _Esolid;oblðWÞ _Eocean;eccðWÞ _Eocean;oblðWÞ Europa 2.02 1011 9.77 1011 1.34 109 7.05 1012 9.70 109 1.47 107 3.1 109 Ganymede 4.67 1011 8.79 109 2.49 108 5.46 1010 1.55 109 1.66 104 1.3 109 Callisto 3.20 1011 2.08 109 9.30”
Long-Term Stability of a Subsurface Ocean on Enceladus (2007, background): “One might imagine that through interactions with other satellites, Enceladus’ eccentricity may have been higher in the past (Meyer and Wisdom, 2007).”