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Modeling stresses on satellites due to nonsynchronous rotation and orbital eccentricity using gravitational potential theory
Abstract The tidal stress at the surface of a satellite is derived from the gravitational potential of the satellite's parent planet, assuming that the satellite is fully differentiated into aExpand
Lunar-forming impacts: High-resolution SPH and AMR-CTH simulations
Abstract We present results of the highest-resolution simulations to date of potential Moon-forming impacts using a Lagrangian, particle-based method (smooth particle hydrodynamics, or SPH) and anExpand
LIMITS ON HEAT TRANSPORT AND RESURFACING RATES DUE TO MOBILE LID CONVECTION BENEATH ENCELADUS’ SOUTH POLAR TERRAIN
Background & Motivation: Cassini CIRS data indicate that Enceladus’ south polar terrain (SPT) has a large endogenic power output PCIRS ≥ 5.8 ± 1.9 GW [1]. Spread over the ~70,000 km region of theExpand
Convection in Enceladus' ice shell: Conditions for initiation
[1] Observations of Enceladus by the Cassini spacecraft indicate that this tiny Saturnian moon is geologically active, with plumes of water vapor and ice particles erupting from its southern polarExpand
Origin of the Ganymede–Callisto dichotomy by impacts during the late heavy bombardment
Jupiter’s large moons Ganymede and Callisto are similar in size and composition, but different in surface and interior characteristics. Simulations with geophysical models of core formation indicateExpand
Constraints on gas giant satellite formation from the interior states of partially differentiated satellites
An icy satellite whose interior is composed of a homogeneous ice/rock mixture must avoid melting during its entire history, including during its formation when it was heated by deposition ofExpand
Enceladus: An Active Cryovolcanic Satellite
Enceladus is one of the most remarkable satellites in the solar system, as revealed by Cassini's detection of active plumes erupting from warm fractures near its south pole. This discovery makesExpand
Heat Transfer in Europa's Icy Shell
TLDR
A meltthrough model for chaos formation on Europa, and thermal and topographic tests of Europa chaos formation models from Galileo E15 observations. Expand
Domes on Europa: The Role of Thermally Induced Compositional Diapirism
The surface of Europa is peppered by topographic domes, interpreted as sites of intrusion and extrusion. Diapirism is consistent with dome morphology, but thermal buoyancy alone cannot produceExpand
Interior Structures and Tidal Heating in the TRAPPIST-1 Planets
With seven planets, the TRAPPIST-1 system has the largest number of exoplanets discovered in a single system so far. The system is of astrobiological interest, because three of its planets orbit inExpand
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