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  2. Eris (dwarf planet) - Wikipedia

    en.wikipedia.org/wiki/Eris_(dwarf_planet)

    Using the 2011 occultation results, Eris has a density of 2.52 ± 0.07 g/cm 3, [g] substantially denser than Pluto, and thus must be composed largely of rocky materials. [12] Models of internal heating via radioactive decay suggest that Eris could have a subsurface ocean of liquid water at the mantle–core boundary. [69]

  3. Portal:Solar System/Selected article - Wikipedia

    en.wikipedia.org/wiki/Portal:Solar_System/...

    A number of faint dust bands and incomplete arcs may exist between the main rings. The rings are extremely dark—the Bond albedo of the rings' particles does not exceed 2%. They are likely composed of water ice with the addition of some dark radiation-processed organics. The majority of Uranus's rings are opaque and only a few kilometres wide.

  4. Geology of solar terrestrial planets - Wikipedia

    en.wikipedia.org/wiki/Geology_of_solar...

    There are indications that Ceres may have a tenuous atmosphere and water frost on the surface. Surface water ice is unstable at distances less than 5 AU from the Sun, so it is expected to vaporize if it is exposed directly to solar radiation. Water ice can migrate from the deep layers of Ceres to the surface, but escapes in a very short time.

  5. Terrestrial planet - Wikipedia

    en.wikipedia.org/wiki/Terrestrial_planet

    [8] [9] Titan even has surface bodies of liquid, albeit liquid methane rather than water. Jupiter's Ganymede, though icy, does have a metallic core like the Moon, Io, Europa, and the terrestrial planets. The name Terran world has been suggested to define all solid worlds (bodies assuming a rounded shape), without regard to their composition. It ...

  6. Planetary surface - Wikipedia

    en.wikipedia.org/wiki/Planetary_surface

    Normally, giant planets are considered to not have a surface, although they might have a solid core of rock or various types of ice, or a liquid core of metallic hydrogen. However, the core, if it exists, does not include enough of the planet's mass to be actually considered a surface.

  7. Water on terrestrial planets of the Solar System - Wikipedia

    en.wikipedia.org/wiki/Water_on_terrestrial...

    The current Venusian atmosphere has only ~200 mg/kg H 2 O(g) in its atmosphere and the pressure and temperature regime makes water unstable on its surface. Nevertheless, assuming that early Venus's H 2 O had a ratio between deuterium (heavy hydrogen, 2H) and hydrogen (1H) similar to Earth's Vienna Standard Mean Ocean Water of 1.6×10 −4, [7] the current D/H ratio in the Venusian atmosphere ...

  8. List of natural satellites - Wikipedia

    en.wikipedia.org/wiki/List_of_natural_satellites

    At least 19 of them are large enough to be gravitationally rounded; of these, all are covered by a crust of ice except for Earth's Moon and Jupiter's Io. [1] Several of the largest ones are in hydrostatic equilibrium and would therefore be considered dwarf planets or planets if they were in direct orbit around the Sun and not in their current ...

  9. Planetary habitability in the Solar System - Wikipedia

    en.wikipedia.org/wiki/Planetary_habitability_in...

    Planetary habitability in the Solar System is the study that searches the possible existence of past or present extraterrestrial life in those celestial bodies. As exoplanets are too far away and can only be studied by indirect means, the celestial bodies in the Solar System allow for a much more detailed study: direct telescope observation, space probes, rovers and even human spaceflight.