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The Astrobiology Primer v2.0. [PDF]
Domagal-Goldman SD +48 more
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Astronomical Observations in Support of Planetary Entry-Probes to the Outer Planets. [PDF]
Buratti BJ +4 more
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Detection of carbon dioxide and hydrogen peroxide on the stratified surface of Charon with JWST. [PDF]
Protopapa S +16 more
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Geologic Constraints on the Formation and Evolution of Saturn's Mid-Sized Moons. [PDF]
Rhoden AR +9 more
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Multiple Probe Measurements at Uranus Motivated by Spatial Variability. [PDF]
Wong MH +3 more
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Dynamical evolution of the Uranian satellite system I.
Sérgio R.A. Gomes +1 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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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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Voyager 2 Photopolarimeter observations of the Uranian satellites
Journal of Geophysical Research: Space Physics, 1987We report the ultraviolet (0.25 µm) and infrared (0.75 µm) geometric albedos, phase curves, and phase coefficients for the large Uranian satellites using full disk photometric observations obtained by the photopolarimeter subsystem during the Voyager 2 encounter with the Uranian system.
Robert M. Nelson +7 more
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Astrometry in the Uranian system of satellites
AIP Conference Proceedings, 2008The predicted occultation between the satellites Miranda(UV) and Oberon(UIV) was observed on July 30, 2007 using SpeX/IRTF system and CODAM‐Paris Observatory facility. Data analysis reveals that the predicted magnitude drop for this phenomenon was overestimated and we establish an upper limit of 0m.05 for the phenomenon, perhaps due to a non‐lambertian
Mirel Birlan +4 more
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