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RE: Miranda
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Gerard Kuiper discoverd Uranus Moon Miranda on February 16, 1948

Uranus Moon Miranda

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Title: A numerical exploration of Miranda's dynamical history
Authors: Emilie Verheylewegen, Benoit Noyelles, Anne Lemaitre

The Uranian satellite Miranda presents a high inclination (4.338) and evidences of resurfacing. It is accepted since 20 years (e.g. Tittemore and Wisdom 1989, Malhotra and Dermott 1990) that this inclination is due to the past trapping into the 3:1 resonance with Umbriel. These last years there is a renewal of interest for the Uranian system since the Hubble Space Telescope permitted the detection of an inner system of rings and small embedded satellites, their dynamics being of course ruled by the main satellites. For this reason, we here propose to revisit the long-term dynamics of Miranda, using modern tools like intensive computing facilities and new chaos indicators (MEGNO and frequency map analysis). As in the previous studies, we find the resonance responsible for the inclination of Miranda and the secondary resonances associated, likely to have stopped the rise of Miranda's inclination at 4.5. Moreover, we get other trajectories in which this inclination reaches 7. We also propose an analytical study of the secondary resonances associated, based on the study by Moons and Henrard (1993).

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Miranda, the smallest and innermost of Uranus' five major moons, was discovered by Gerard Kuiper on February 16, 1948.



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Verona Rupes
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Verona Rupes is a cliff on Miranda, a moon of Uranus. The cliff face has been estimated to be from 5 kilometres to 10 kilometres high, which makes it the tallest known cliff in the solar system.
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Miranda
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Miranda is the smallest and innermost of Uranus' five major moons.
It was discovered by Gerard Kuiper on February 16, 1948 at McDonald Observatory. It was named after Miranda from William Shakespeare's play The Tempest by Kuiper in his report of the discovery.

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