Dione (moon)

Last updated
Dione
Dione in natural light (cropped).jpg
Dione photographed in natural light by the
Cassini spacecraft in 2008
Discovery
Discovered by Giovanni Cassini
Discovery dateMarch 21, 1684
Designations
Designation
Saturn IV
Pronunciation /dˈn/ [1]
Named after
Διώνη Diōnē
Adjectives Dionean [2] /dəˈnən/ [3]
Orbital characteristics
377396 km
Eccentricity 0.0022 [4]
2.736915 d [4]
Inclination 0.019° (to Saturn's equator)
Satellite of Saturn
Physical characteristics
Dimensions1128.8×1122.6×1119.2 km [5]
Mean diameter
1122.8±0.8 km [5]
Mean radius
561.4±0.4 km
3964776.51 km2 [6]
Mass (1.095452±0.000168)×1021 kg [7] (1.834×104 Earths)
Mean density
1.478±0.003 g/cm³ [5]
0.232 m/s2
0.51 km/s
2.736915 d
(synchronous)
zero
Albedo 0.998±0.004 (geometric) [8]
Temperature 87 K (−186°C)
10.4 [9]

    Dione ( /dˈni/ ) is a moon of Saturn. It was discovered by Italian astronomer Giovanni Domenico Cassini in 1684. [10] It is named after the Titaness Dione of Greek mythology. It is also designated Saturn IV.

    Contents

    Name

    Giovanni Domenico Cassini named the four moons he discovered (Tethys, Dione, Rhea and Iapetus) Sidera Lodoicea ("the stars of Louis") to honor king Louis XIV. Cassini found Dione in 1684 using a large aerial telescope he set up on the grounds of the Paris Observatory. [11] The satellites of Saturn were not named until 1847, when William Herschel's son John Herschel published Results of Astronomical Observations made at the Cape of Good Hope, suggesting that the names of the Titans (sisters and brothers of Cronus) be used. [12]

    Orbit

    Dione orbits Saturn with a semimajor axis about 2% less than that of the Moon. However, reflecting Saturn's greater mass (95 times that of Earth), Dione's orbital period is one tenth that of the Moon. Dione is currently in a 1:2 mean-motion orbital resonance with moon Enceladus, completing one orbit of Saturn for every two orbits completed by Enceladus. This resonance maintains Enceladus's orbital eccentricity (0.0047), providing a source of heat for Enceladus's extensive geological activity, which shows up most dramatically in its cryovolcanic geyser-like jets. [13] The resonance also maintains a smaller eccentricity in Dione's orbit (0.0022), tidally heating it as well. [14]

    Dione has two co-orbital, or trojan, moons, Helene and Polydeuces. They are located within Dione's Lagrangian points L4 and L5, 60 degrees ahead of and behind Dione respectively. A leading co-orbital moon twelve degrees ahead of Helene was reported by Stephen P. Synnott in 1982. [15] [16]

    Physical characteristics and interior

    Size comparison of Earth, the Moon, and Dione. Dione, Earth & Moon size comparison.jpg
    Size comparison of Earth, the Moon, and Dione.

    At 1122 km (697 mi) in diameter, Dione is the 15th largest moon in the Solar System, and is more massive than all known moons smaller than itself combined. [17] About two thirds of Dione's mass is water ice, and the remaining is a dense core, probably silicate rock. [18]

    Data gathered by Cassini indicates that Dione has an internal liquid salt water ocean (a situation similar to that of its orbital resonance partner, Enceladus). [19] Downward bending of the surface associated with the 1.5 km high ridge Janiculum Dorsa can most easily be explained by the presence of such an ocean. [20] [21] Gravity and shape data point to a 99 ± 23 km thick ice shell crust on top of a 65 ± 30 km deep internal liquid water global ocean. [22] [23] Neither moon has a shape close to hydrostatic equilibrium; the deviations are maintained by isostasy. Dione's ice shell is thought to vary in thickness by less than 5%, with the thinnest areas at the poles, where tidal heating of the crust is greatest. [23]

    Though somewhat smaller and denser, Dione is otherwise very similar to Rhea. They both have similar albedo features and varied terrain, and both have dissimilar leading and trailing hemispheres. Dione's leading hemisphere is heavily cratered and is uniformly bright. Its trailing hemisphere, however, contains an unusual and distinctive surface feature: a network of bright ice cliffs.

    Scientists recognise Dionean geological features of the following types:

    Ice cliffs (formerly 'wispy terrain')

    Fractures bisecting older craters on Dione. Those running from upper right to lower left are the Carthage Fossae, whereas Pactolus Catena runs more horizontally at lower right. Dione Carthage Linea.jpg
    Fractures bisecting older craters on Dione. Those running from upper right to lower left are the Carthage Fossae, whereas Pactolus Catena runs more horizontally at lower right.

    When the Voyager space probe photographed Dione in 1980, it showed what appeared to be wispy features covering its trailing hemisphere. The origin of these features was mysterious, because all that was known was that the material has a high albedo and is thin enough that it does not obscure the surface features underneath. One hypothesis was that shortly after its formation Dione was geologically active, and some process such as cryovolcanism resurfaced much of its surface, with the streaks forming from eruptions along cracks in the Dionean surface that fell back as snow or ash. Later, after the internal activity and resurfacing ceased, cratering continued primarily on the leading hemisphere and wiped out the streak patterns there.

    This hypothesis was proven wrong by the Cassini probe flyby of December 13, 2004, which produced close-up images. These revealed that the 'wisps' were, in fact, not ice deposits at all, but rather bright ice cliffs created by tectonic fractures (chasmata). Dione has been revealed as a world riven by enormous fractures on its trailing hemisphere.

    The Cassini orbiter performed a closer flyby of Dione at 500 km (310 mi) on October 11, 2005, and captured oblique images of the cliffs, showing that some of them are several hundred metres high.

    Linear features

    Dione features linear 'virgae' that are up to hundreds of km long but less than 5 km wide. These lines run parallel to the equator and are only apparent at lower latitudes (at less than 45° north or south); similar features are noted on Rhea. They are brighter than everything around them and appear to overlay other features such as ridges and craters, indicating they are relatively young. It has been proposed that these lines are of exogenic origin, as the result of the emplacement of material across the surface by low‐velocity impacts of material sourced from Saturn's rings, co‐orbital moons, or closely approaching comets. [24]

    Craters

    Dione before Enceladus PIA18345-SaturnMoons-DioneEnceladus-CassiniHuygens-20150908.jpg
    Dione before Enceladus

    Dione's icy surface includes heavily cratered terrain, moderately cratered plains, lightly cratered plains, and areas of tectonic fractures. The heavily cratered terrain has numerous craters greater than 100 kilometres (62 mi) in diameter. The plains areas tend to have craters less than 30 kilometres (19 mi) in diameter. Some of the plains are more heavily cratered than others. Much of the heavily cratered terrain is located on the trailing hemisphere, with the less cratered plains areas present on the leading hemisphere. This is the opposite of what some scientists expected; Shoemaker and Wolfe [25] proposed a cratering model for a tidally locked satellite with the highest cratering rates on the leading hemisphere and the lowest on the trailing hemisphere. This suggests that during the period of heavy bombardment, Dione was tidally locked to Saturn in the opposite orientation. Because Dione is relatively small, an impact causing a 35 kilometer crater could have spun the satellite. Because there are many craters larger than 35 kilometres (22 mi), Dione could have been repeatedly spun during its early heavy bombardment. The pattern of cratering since then and the bright albedo of the leading side suggests that Dione has remained in its current orientation for several billion years.

    Like Callisto, Dione's craters lack the high-relief features seen on the Moon and Mercury; this is probably due to slumping of the weak icy crust over geologic time.

    Atmosphere

    Cassini enhanced-color composite of Dione, showing the darker, fractured terrain of the trailing hemisphere. The Padua Chasmata trace an arc on the left, interrupted near the top by a central peak crater. Dione color.jpg
    Cassini enhanced-color composite of Dione, showing the darker, fractured terrain of the trailing hemisphere. The Padua Chasmata trace an arc on the left, interrupted near the top by a central peak crater.

    On April 7, 2010, instruments on board the unmanned Cassini probe, which flew by Dione, detected a thin layer of molecular oxygen ions (O+
    2
    ) around Dione, so thin that scientists prefer to call it an exosphere rather than a tenuous atmosphere. [26] [27] The density of molecular oxygen ions determined from the Cassini plasma spectrometer data ranges from 0.01 to 0.09 per cm3. [27] [28]

    The Cassini probe instruments were unable to directly detect water from the exosphere due to high background levels, [27] but it seems that highly charged particles from the planet's powerful radiation belts could split the water in the ice into hydrogen and oxygen. [26]

    Exploration

    Dione was first imaged by the Voyager space probes. It has also been probed five times from close distances by the Cassini orbiter. There was a close targeted flyby, at a distance of 500 km (310 mi) on 11 October 2005; [29] another flyby was performed on 7 April 2010 also at a distance of 500 km. [30] A third flyby was performed on 12 December 2011 at a distance of 99 km (62 mi). The following flyby was on 16 June 2015 at a distance of 516 km (321 mi), [31] and the last Cassini flyby was performed on 17 August 2015 at a distance of 474 km (295 mi). [32] [33]

    In May 2013, it was announced that NASA's spacecraft Cassini had provided scientists with evidence that Dione is more active than previously realized. Using topographic data, NASA teams deduced that crustal depression associated with a prominent mountain ridge on the leading hemisphere is best explained if there was a global subsurface liquid ocean like that of Enceladus. [20] [34] [35] The ridge Janiculum Dorsa has a height of 1 to 2 km (0.6 to 1.2 miles); Dione's crust seems to pucker 0.5 km (0.3 miles) under it, suggesting that the icy crust was warm when the ridge formed, probably due to the presence of a subsurface liquid ocean, which increases tidal flexing. [36]

    Dione and the rings of Saturn
    PIA18344-SaturnMoon-Dione-Cassini-20150817.jpg
    PIA18346-SaturnMoon-Dione-20150815.jpg
    Dione and Saturn.jpg
    Color map of Dione PIA18434 Nov. 2014.jpg
    Color map of Dione PIA18434 Nov. 2014.jpg
    Enhanced-color map (25.9 MB); the trailing hemisphere (left) may be darkened by magnetospheric radiation; the leading hemisphere is coated with E Ring deposits.
    Color Dione polar maps PIA18434 Nov. 2014.jpg
    Color Dione polar maps PIA18434 Nov. 2014.jpg
    Enhanced-color maps: northern and southern hemispheres
    PIA18434-SaturnMoon-Dione-20141104-fig2.jpg
    PIA18434-SaturnMoon-Dione-20141104-fig2.jpg
    Enhanced-color maps: trailing and leading hemispheres
    Crescent Dione from Cassini, October 11, 2005. The crater near the limb at top is Alcander, with larger crater Prytanis adjacent to its left. At lower right, several of the Palatine Chasmata fractures are visible, one of which can be seen bisecting the smaller craters Euryalus (right) and Nisus. Crescent Dione.jpg
    Crescent Dione from Cassini , October 11, 2005. The crater near the limb at top is Alcander, with larger crater Prytanis adjacent to its left. At lower right, several of the Palatine Chasmata fractures are visible, one of which can be seen bisecting the smaller craters Euryalus (right) and Nisus.

    See also

    Related Research Articles

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    Exploration of Saturn Overview of the exploration of Saturn

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