Results from Hammond and Barr’s simulations provide a preliminary set of answers that strive to unlock the mysteries of Miranda’s bizarre appearance. “Simulations that match the thermal gradient from flexure have total power outputs of close to 10 GW, somewhat larger than the total power we predict could be generated during orbital resonance.” Hammond and Barr’s simulation results indicate almost twice that amount of power would have been created: Using Saturn’s moon Enceladus as a baseline due to its similarity in size, composition, and orbital frequency to Miranda, original calculations estimate that as much as 5 GW of tidal dissipation power could be generated. Models that account for the possible distribution of tidal heat ing can even match the precise locations of the coronae, after a reorientation of 60°.” “We find that convection in Miranda’s ice shell powered by tidal heating can generate the global distribution of coronae, the concentric orientation of sub-parallel ridges and troughs, and the thermal gradient implied by flexure. In their paper titled, “Global Resurfacing of Uranus’s Moon Miranda by Convection,” Hammond and Barr summarize their results as follows: Barr have produced results that are consistent with the three coronae seen on Miranda. Scientists believe that tidal warming played an important role in the formation of the coronae, but the process by which this internal heating led to these features has remained unclear.Įxtensive 3D computer simulations conducted by Brown University’s Noah P. Based on this premise, the question is then raised as to what mechanism/processes in Miranda’s past warmed its interior sufficiently to produce warm, sub-surface fluids that resulted in coronae formation. As the edges of the dome cool, the center collapses and warm fluid leak out its sides, forming a crown-like structure, or corona. Coronae were first identified on Venus in 1983 by Venera 15/16 radar imaging equipment.Ī leading theory about their formation has been that they form when warm, sub-surface fluids rise to the surface and form a dome. Although it is only 293 miles (471 kilometers) in diameter (approximately one-seventh that of Earth’s moon,) it has one of the strangest and most varied landscapes in our Solar System.Ĭentral to the new research was analysis of three very large, geometric shaped features known as coronae, which are only found on one other planetary body. Miranda was discovered in 1948 by Gerard Kuiper. To date, Venus and Miranda are the only bodies in our solar system on which coronae have been observed. Three large, geometric-shaped features called coronae are visible on Miranda. First thought to be the result of a catastrophic impact, disintegration, and subsequent reassembly, scientists now believe that some of Miranda’s features might have been influenced by Uranus itself, and are the result of convection: thermally-induced resurfacing from tidal forces from the planet. Over the years, various hypotheses have been presented in an attempt to account for Miranda’s enigmatic appearance. Plus, it has incredibly diverse surface features including canyons up to 12 times deeper than Earth’s Grand Canyon, impact craters, cliffs, and parallel grooves called sulci. It does not store any personal data.Miranda, the innermost of Uranus’ five moons, has a “Frankenstein”-like appearance: it looks as though it was pieced together from parts that didn’t quite fit together properly. The cookie is set by the GDPR Cookie Consent plugin and is used to store whether or not user has consented to the use of cookies. The cookie is used to store the user consent for the cookies in the category "Performance". This cookie is set by GDPR Cookie Consent plugin. The cookie is used to store the user consent for the cookies in the category "Other.
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