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Orbital evolution of the main Uranian satellites
, 2011 Since Voyager 2 space mission, we know some properties of the main Uranian satellites (Miranda, Ariel, Umbriel, Titania, Oberon): on the one hand, we observe an important resurfacing of both Miranda and Ariel, and on the other hand some strangenesses in the orbital elements such as the anomalously high inclinaison of Miranda or the anomalously high ...
Verheylewegen, E., Noyelles, Benoît
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Mutual events of the uranian satellites 2006–2010
Icarus, 2005Abstract The upcoming crossing of the Sun and the Earth through the equatorial plane of the planet Uranus presents an opportunity to observe mutual eclipses and occultations of the uranian satellites. We present predictions for 321 such events from 2006 to 2010. 230 of these events are “nominal” i.e. they are predicted to occur based on the currently
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Mutual Events in the Uranian satellite system in 2007
, 2008 The equinox time on the giant planets When the Sun crosses the equatorial plane of a giant planet, it is the equinox time occurring every half orbit of the planet, i.e. every 6 years for Jupiter, 14 years for Saturn, 42 years for Uranus and 82 years for Neptune. Except Neptune, each planet have several major satellites orbiting in the equatorial plane,
Arlot, Jean-Eudes
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Post eclipse thermal response of Uranian satellites with SINFONI: a status report .
Memorie della Società Astronomica Italiana. Supplementi, 2008 We report on the status of a project to measure eclipse-induced changes in surface temperature on the major Uranian satellites. Such measurements enable a uniquely direct determination of the thermal inertia, a measure of the resistance to changes in surface temperature.
Maris, M. +8 more
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Monthly Notices of the Royal Astronomical Society, 2013 International audienceAn observational campaign of the five Uranian major satellites was carried out during the period 1998-2007. A total of 2358 satellite observations in 1025 CCD frames were taken at two observational stations near Beijing and Shanghai
R C Qiao, G Dourneau, Z H Tang
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Icarus, 2013 a b s t r a c t Dust grains generated by the Uranian irregular satellites will undergo chaotic large-amplitude eccentricity oscillations under the simultaneous action of radiation forces and the highly misaligned quadrupole potentials of the oblate ...
Daniel Tamayo +2 more
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The enigma of the Uranian satellites' orbital eccentricities
Icarus, 1985The eccentricity decay times for the Uranian satellites are calculated using recent observations (Brown et al., 1982) of the diameters and orbital elements of the satellites and assuming reasonable dissipation functions and rigidities for icy satellites.
Steven W. Squyres +2 more
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Surface properties and photometry of the Uranian satellites
Icarus, 1990Voyager photographic images and photopolarimetric experiment observations have been used to obtain the spectral geometric and Bond albedos, phase integrals, color-dependent phase coefficients, and integrated solar phase-curve parameters of the five Uranian satellites Miranda, Ariel, Umbriel, Titania, and Oberon. While the results obtained confirm those
Bonnie Buratti +2 more
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Orbital Stability of the Uranian Satellite System☆
Icarus, 1997Abstract We have numerically integrated approximately 500 systems of mutually gravitating bodies which were based on subsets of the uranian satellite system. In each run within a set, the satellite masses were initially multiplied by a common mass enhancement factormf.
M DUNCAN, J LISSAUER
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Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 2020
Newly processed global imaging and topographic mapping of Uranus's five major satellites reveal differences and similarities to mid-sized satellites at Saturn and Pluto. Three modes of internal heat redistribution are recognized. The broad similarity of Miranda's three oval resurfacing zones to those mapped on Enceladus and (subtly) on Dione are likely
Paul M. Schenk, Jeffrey M. Moore
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Newly processed global imaging and topographic mapping of Uranus's five major satellites reveal differences and similarities to mid-sized satellites at Saturn and Pluto. Three modes of internal heat redistribution are recognized. The broad similarity of Miranda's three oval resurfacing zones to those mapped on Enceladus and (subtly) on Dione are likely
Paul M. Schenk, Jeffrey M. Moore
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