Tidal stress modeling of Ganymede: Strike-slip tectonism and Coulomb failure

Cameron, M. E.; Smith-Konter, B. R.; Collins, G. C.; Patthoff, D. A.; Pappalardo, R. T.

doi:10.1016/j.icarus.2018.09.002

Cited by 17 publications

(21 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Bottom right, en-echelon structures in the light subdued material found within Transitional Terrain (173°E, 32°N). In Gray the thickness predicted by Equation 8 (c) vs. the prediction given by Cameron et al, (2019) (d). Arrows indicate inferred shear sense assuming a transtensional origin, where bold red lines are features of interests, thin red lines are craters and features outside of the relevant zone, and green lines are scarps (ticks point downslope) (from Cameron et al, (2018), Deremer et al, (2003)).…”

Section: Ganymedementioning

confidence: 99%

Assessing the brittle crust thickness from strike-slip fault segments on Earth, Mars and Icy moons

et al. 2021

View full text Add to dashboard Cite

Section: Ganymedementioning

confidence: 99%

Assessing the brittle crust thickness from strike-slip fault segments on Earth, Mars and Icy moons

et al. 2021

View full text Add to dashboard Cite

“…Table 2 of Hurford et al (2018) lists η = 10 21 , 10 21 , 10 20 and 10 14 Pa•s respectively for Europa's iron core, brittle ice layer, silicate mantle, and ductile ice layer. Cameron et al (2019) give similar values for Ganymede, whereas Table 1 of Patthoff et al (2019) lists η = 10 28 , 10 22 , 10 14 Pa•s respectively for the core, upper ice layer and lower ice layer of Enceladus. The latter two values actually were chosen from wide ranges previously reported in the literature of 10 19 − 10 26 Pa•s for the upper ice layer and 10 12 − 10 17 Pa•s for the lower ice layer.…”

Section: Variable Initial Conditions and Parameters Across Simulationsmentioning

confidence: 84%

Orbital relaxation and excitation of planets tidally interacting with white dwarfs

Veras

Efroimsky

Макаров

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Observational evidence of white dwarf planetary systems is dominated by the remains of exo-asteroids through accreted metals, debris discs, and orbiting planetesimals. However, exo-planets in these systems play crucial roles as perturbing agents, and can themselves be perturbed close to the white dwarf Roche radius. Here, we illustrate a procedure for computing the tidal interaction between a white dwarf and a near-spherical solid planet. This method determines the planet's inward and/or outward drift, and whether the planet will reach the Roche radius and be destroyed. We avoid constant tidal lag formulations and instead employ the self-consistent secular Darwin-Kaula expansions from Boué & Efroimsky (2019), which feature an arbitrary frequency dependence on the quality functions. We adopt wide ranges of dynamic viscosities and spin rates for the planet in order to straddle many possible outcomes, and provide a foundation for the future study of individual systems with known or assumed rheologies. We find that: (i) massive Super-Earths are destroyed more readily than minor planets (such as the ones orbiting WD 1145+017 and SDSS J1228+1040), (ii) low-viscosity planets are destroyed more easily than high-viscosity planets, and (iii) the boundary between survival and destruction is likely to be fractal and chaotic.

show abstract

“…We assume a nominal depth of analysis of z = 100 m and a relatively low coefficient of friction of μ f = 0.2. Cameron et al (2019) found that Coulomb failure is not achieved when considering a present‐day eccentricity because the present‐day eccentricity produces diurnal tidal shear tractions (<5 kPa) that are an order of magnitude smaller than the frictional stresses resisting slip (~30–80 kPa for a range of μ f ).…”

Section: Regional Resultsmentioning

confidence: 99%

“…This approach has been used for predicting failure on icy satellite faults (Hurford et al, 2007; Nimmo et al, 2007; Smith‐Konter & Pappalardo, 2008). To investigate diurnal stresses, we compute the Coulomb stresses induced by present‐day low, and past high, eccentricities at depth ( z = 100 m increments) by resolving the raw stresses generated by SatStress on the fault plane as a function of the fault orientation, coefficient of friction of ice, and overburden pressure (Cameron et al, 2019). We calculate the Coulomb stress as

τ_{c} = (||, τ_{s}) - μ_{f} ()(, σ_{n} + italicρgz),

where τ c is the Coulomb stress, τ s is the diurnal shear traction on the fault, μ f is the effective coefficient of friction (based on lab‐derived values from Fortt & Schulson, 2007; Schulson & Fortt, 2012), σ n is the normal stress, ρ is the density, g is gravitational acceleration, and z is depth.…”

Section: Tidal Stress and Coulomb Failure Modelingmentioning

confidence: 99%

Ganymede, Then and Now: How Past Eccentricity May Have Altered Tidally Driven Coulomb Failure

et al. 2020

Self Cite

View full text Add to dashboard Cite

Laplace‐like resonances among Ganymede, Europa, and Io may have once led Ganymede to have an eccentricity (presently e = 0.0013) as high as ~0.07 (Showman & Malhotra, 1997, https://doi.org/10.1006/icar.1996.5669). While diurnal stresses at Ganymede today are small (less than 10 kPa), a previous period of higher eccentricity may have allowed for an order of magnitude increase in the diurnal tidal stresses that could drive fault initiation and result in a past period of active tectonism. To investigate the role of tidal stresses on faulting, we use the numerical model SatStress (Wahr et al., 2009, https://doi.org/10.1016/j.icarus.2008.11.002) to calculate diurnal tidal stresses on Ganymede's surface assuming e = 0.05, representative of a more eccentric orbit in Ganymede's past. We resolve normal and shear stresses onto discrete mapped fault segments and assess Coulomb failure criteria along three inferred shear zones on Ganymede's surface: Dardanus Sulcus, Tiamat Sulcus, and Nun Sulci. While Coulomb failure is not expected from diurnal stressing at any of the three shear zones for a diurnal model of present‐day (low) eccentricity, we do predict Coulomb failure for a past, high eccentricity case, in isolated diurnal slip windows and limited to very shallow depths (~100 to 250 m). In these cases, this model may provide an alternative to invoking additional stresses such as nonsynchronous rotation or true polar wander, as in previous studies (Cameron et al., 2019, https://doi.org/10.1016/j.icarus.2018.09.002). Additionally, this model is in general agreement with the sense of inferred shear from imagery and structural mapping.

show abstract

Tidal stress modeling of Ganymede: Strike-slip tectonism and Coulomb failure

Cited by 17 publications

References 62 publications

Assessing the brittle crust thickness from strike-slip fault segments on Earth, Mars and Icy moons

Assessing the brittle crust thickness from strike-slip fault segments on Earth, Mars and Icy moons

Orbital relaxation and excitation of planets tidally interacting with white dwarfs

Ganymede, Then and Now: How Past Eccentricity May Have Altered Tidally Driven Coulomb Failure

Contact Info

Product

Resources

About