Lunar rotational dissipation in solid body and molten core

By James G. Williams, D. Boggs, C. F. Yoder, J. T. Ratcliff, J. Dickey. 2001

370 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/9f708f8ed22a653606241abbee73c149efee121d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Molecular Biology

Citations in the corpus

A 3‐D numerical study of the thermal evolution of the Moon after cumulate mantle overturn: The importance of rheology and core solidification (2013, background): “We now consider a case of 300 km radius core (H50E100V5e20C300; the light blue curve in Figure 7b), a possible lower bound for lunar core (Table 2) [Williams et al., 2001].”
Joint inversion of seismic and gravity data for lunar composition and thermal state (2007, background): “Concerning the core, current consensus favours a small ( Williams et al. 2001; Khan et al. 2004), in line with the prevailing model for the origin of the Moon (Canup 2004).”
Long term evolution and chaotic diffusion of the insolation quantities of Mars (2004, neutral): “…O ( τ 2 (cid:15) 2 ), and even O ( τ 8 )+ O ( τ 4 (cid:15) 2 ) when the correction step is added, while the same quantity is of the order O ( τ 2 ) in the widely used symplectic integrator of Wisdom and Holman (1991), and O ( τ n ) + O ( τ 2 (cid:15) 2 ) with the correctors of Wisdom et al. (1996).”
The Physics of Bodily Tides in Terrestrial Planets, and the Appropriate Scales of Dynamical Evolution (2007, neutral): “S = − 3 k2 R 5 G (Mo + m) m ∆t Mo a7 (n − ωp) , (35)”
Bodily tides near spin–orbit resonances (2011, methodology): “Fitting of the LLR data to the scaling law (75) was carried out by Williams et al. (2001) who demonstrated that the lunar mantle possesses quite an abnormal value of the exponent: −0.19. A later reexamination in Williams et al. (2008) gave a less embarrassing value, −0.”
Lunar interior properties from the GRAIL mission (2014, methodology): “The fluid rotation is not synchronous [Williams et al., 2001], and the fluid torques act against synchronous rotation of the inner core, but the influence of the fluid is very weak compared with the gravitational torques.”
Dipole moment scaling for convection-driven planetary dynamos (2005, neutral): “Jupiter 2.42 16.0 0.16 0.1 18,000.0 100 18.0 [43–45] Saturn 2.25 8.5 0.16 0.1 580.0 50 7.0 [46,47] Uranus 1.39 4.9 0.18 0.03 50.0 20 5.0 [48] Neptune 1.49 4.5 0.18 0.03 24.0 20 5.0 [49] Moona 0.07 0.12 0.9 1.0 0.001 0.3 0.12 [ 50 ]”
Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios (2004, background): “radius between 0 and 375 km (upper bound taken from Williams et al. [2001]), and a crustal thickness range between 43 and 53 km (using the seismic constraints of”
Farside deep moonquakes and deep interior of the Moon (2005, methodology): “The Moon is no exception in this respect, and many attempts have been made using various techniques, including electromagnetic sounding [e.g., Hood et al., 1999] and laser ranging measurements [e.g., Williams et al., 2001 ], with limited success.”
Tidal torques: a critical review of some techniques (2008, background): “Other possibilities include introducing an apparent mean motion, i.e., defining n either as the mean-anomaly rate dM/dt , or as the mean-longitude rate dL/dt = dΩ/dt + dω/dt + dM/dt (as was done by Williams et al. 2001).”
High‒degree gravity models from GRAIL primary mission data (2013, methodology): “Together with the low-degree gravity field coefficients, the Love numbers can be used to constrain models of the deep lunar interior [e.g., Williams et al., 2001; Williams, 2007; Zhong et al., 2012].”