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Dione (moon)

Not to be confused with the asteroid called 106 Dione.
For other uses, see [[Dione (disambiguation)#REDIRECTmw:Help:Magic words#Other
This page is a soft redirect.Dione]].
Cassini view of Dione's leading hemisphere. The large craters on or near the terminator are (from bottom to top) Evander, Erulus, Lagus and Sagaris. The Palatine Chasmata fractures stretch across the lower right limb, and the trough Aufidus Catena extends along the bottom near the south pole.
Discovered by Giovanni Cassini
Discovery date March 21, 1684
Saturn IV
Adjectives Dionean
Orbital characteristics
377396Lua error: Unmatched close-bracket at pattern character 67.
Eccentricity 0.0022[1]
2.736915Lua error: Unmatched close-bracket at pattern character 67.[1]
Inclination 0.019° (to Saturn's equator)
Satellite of Saturn
Physical characteristics
Dimensions 1128.8 × 1122.6 × 1119.2 km[2]
Mean radius
561.4±0.4Lua error: Unmatched close-bracket at pattern character 67.[2]
3964776.51Lua error: Unmatched close-bracket at pattern character 67.[3]
Mass (1.095452±0.000168)×1021Lua error: Unmatched close-bracket at pattern character 67.[4] (3.28×104 Earths)
Mean density
1.478±0.003Lua error: Unmatched close-bracket at pattern character 67.[2]
0.233 m/s2
0.51 km/s
2.736915Lua error: Unmatched close-bracket at pattern character 67.
Albedo 0.998±0.004 (geometric)[5]
Temperature 87 K (−186°C)
10.4 [6]

Dione (/dˈni/;[7] Greek: Διώνη) is a moon of Saturn discovered by Italian astronomer Giovanni Domenico Cassini in 1684.[8] It is named after the Titaness Dione of Greek mythology. It is also designated Saturn IV.


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 using a large aerial telescope he set up on the grounds of the Paris Observatory.[9] 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.[10]


Dione orbits Saturn with a semimajor axis about 2% less than that of the Moon. However, reflecting Saturn's greater mass, 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.[11]

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.

Physical characteristics

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

At Script error: No such module "convert". in diameter, Dione is the 15th largest moon in the Solar System, and is more massive than all known moons smaller than itself combined.[12] It is composed primarily of water ice, but as the third densest of Saturn's moons (after Enceladus and Titan, whose density is increased by gravitational compression) it must have a considerable fraction (~46%) of denser material like silicate rock in its interior.[citation needed]

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:

<center>Enhanced-color map (25.9 MB) - leading hemisphere (right) coated with E Ring deposits - trailing hemisphere may be darkened by magnetospheric radiation.</center>
<center>Enhanced-color maps
north and south hemispheres</center>
<center>Enhanced-color maps
trailing and leading hemispheres</center>
File: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.

The ice cliffs (formerly 'wispy terrain')

File: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 Dione's surface that fell back to the surface 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 theory 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 Script error: No such module "convert". on October 11, 2005, and captured oblique images of the cliffs, showing that some of them are several hundred metres high.


File:Dione and Saturn.jpg
Dione against the shadow of Saturn's rings.

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 Script error: No such module "convert". in diameter. The plains areas tend to have craters less than Script error: No such module "convert". 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[13] 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 Script error: No such module "convert"., 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.


On April 7, 2010, instruments on board the unmanned Cassini probe, which flew by Dione, detected a thin layer of molecular oxygen ions (Template:Chem/atomTemplate:Chem/atomTemplate:Chem/atom) around Dione, so thin that scientists prefer to call it an "exosphere" rather than a tenuous atmosphere.[14][15] The density of molecular oxygen ions determined from the Cassini plasma spectrometer data ranges from 0.01 to 0.09 per cm3.[15][16]

The Cassini probe instruments were unable to directly detect water from the exosphere due to high background levels,[15] but it seems that highly charged particles from the planets' powerful radiation belts could split the water in the ice into hydrogen and oxygen.[14]


File: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 central peak crater Ascanius. The Janiculum Dorsa extend along the upper right terminator. Near the lower left limb is the small crater Cassandra with its prominent ray system.

Dione was first imaged by the Voyager space probes. It has also been probed three times from closer distances by the Cassini orbiter. There was one close targeted fly-by, at a distance of 500 km, on October 11, 2005; another similarly close fly-by was performed on April 7, 2010. A third fly-by was performed on December 12, 2011, at an altitude of 99 km.

In May 2013, NASA's spacecraft Cassini provided scientists with new evidence that the Saturian moon Dione could be more active than previously predicted. It is thought that Dione could be a fossil of the activity that Cassini previously discovered spraying from Enceladus, another moon of Saturn. Using stereo-generated topography images, some NASA teams suspect certain flexures across a prominent ridge on the leading hemisphere that would only be possible if there was a subsurface liquid ocean.[17][18][19] This is derived from observations and models of the mountain Janiculum Dorsa. This mountain 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 the mountain, suggesting that the icy crust was warm when the ridge formed, and the best way to get that heat is if Dione had a subsurface ocean.[20] Dione also gets heated by tidal heating as it gets closer to and farther from Saturn in its orbit.[21]

Cassini will perform its next flyby of Dione on 16 June 2015 at a distance of Script error: No such module "convert"..[22]


See also


  1. ^ a b[dead link] Retrieved on 05-21-07
  2. ^ a b c Roatsch, T.; Jaumann, R.; Stephan, K.; Thomas, P. C. (2009). "Cartographic Mapping of the Icy Satellites Using ISS and VIMS Data". Saturn from Cassini-Huygens. pp. 763–781. ISBN 978-1-4020-9216-9. doi:10.1007/978-1-4020-9217-6_24.  edit
  3. ^ Phil Davis? (April 1, 2011). "Solar System Exploration: Planets: Saturn: Moons: Dione: Facts & Figures". NASA. Retrieved March 24, 2013. 
  4. ^ Jacobson, R. A.; Antreasian, P. G.; Bordi, J. J.; Criddle, K. E.; Ionasescu, R.; Jones, J. B.; Mackenzie, R. A.; Meek, M. C.; Parcher, D.; Pelletier, F. J.; Owen, Jr., W. M.; Roth, D. C.; Roundhill, I. M.; Stauch, J. R. (December 2006). "The Gravity Field of the Saturnian System from Satellite Observations and Spacecraft Tracking Data". The Astronomical Journal 132 (6): 2520–2526. Bibcode:2006AJ....132.2520J. doi:10.1086/508812.  edit
  5. ^ Verbiscer, A.; French, R.; Showalter, M.; Helfenstein, P. (9 February 2007). "Enceladus: Cosmic Graffiti Artist Caught in the Act". Science 315 (5813): 815. Bibcode:2007Sci...315..815V. PMID 17289992. doi:10.1126/science.1134681. Retrieved 20 December 2011.  (supporting online material, table S1) edit
  6. ^ Observatorio ARVAL (April 15, 2007). "Classic Satellites of the Solar System". Observatorio ARVAL. Retrieved 2011-12-17. 
  7. ^ In USA dictionary transcription, US dict: dī·ō′·nē.
  8. ^ Cassini, G. D. (1686–1692). "An Extract of the Journal Des Scavans. Of April 22 st. N. 1686. Giving an Account of Two New Satellites of Saturn, Discovered Lately by Mr. Cassini at the Royal Observatory at Paris". Philosophical Transactions of the Royal Society of London 16 (179–191): 79–85. JSTOR 101844. doi:10.1098/rstl.1686.0013.  edit
  9. ^ Fred William Price – The planet observer's handbook – page 279
  10. ^ As reported by William Lassell, Monthly Notices of the Royal Astronomical Society, Vol. 8, No. 3, pp. 42–43 (January 14, 1848)
  11. ^ Porco, C. C.; Helfenstein, P.; Thomas, P. C.; Ingersoll, A. P.; Wisdom, J.; West, R.; Neukum, G.; Denk, T.; Wagner, R. (10 March 2006). "Cassini Observes the Active South Pole of Enceladus". Science 311 (5766): 1393–1401. Bibcode:2006Sci...311.1393P. PMID 16527964. doi:10.1126/science.1123013.  edit
  12. ^ See note g Triton (moon)#Notes
  13. ^ Shoemaker, E. M.; and Wolfe, R. F.; Cratering time scales for the Galilean satellites, in Morrison, D., editor; Satellites of Jupiter, University of Arizona Press, Tucson (AZ) (1982), pp. 277–339
  14. ^ a b Ghosh, Pallab (2 March 2012). "Oxygen envelops Saturn's icy moon". BBC News. Retrieved 2012-03-02. 
  15. ^ a b c Robert L. Tokar; Robert E. Johnson; Michelle F. Thomsen; Edward C. Sittler; Andrew J Coates et al. (10 January 2012). "Detection of Exospheric O2+ at Saturn's Moon Dione". Geophysical Research Letters. Bibcode:2012GeoRL..3903105T. doi:10.1029/2011GL050452. Retrieved 2012-03-02. 
  16. ^ Sven Simon; Joachim Saur; itz M. Neubauer; Alexandre Wennmacher; Michele K. Dougherty (2011). "Magnetic signatures of a tenuous atmosphere at Dione". Geophysical Research Letters 38 (L15102): 5. Bibcode:2011GeoRL..3815102S. doi:10.1029/2011GL048454. Retrieved 2012-03-02. 
  17. ^ Hammond, N. P.; Phillips, C. B.; Nimmo, F.; Kattenhornd, S. A. (March 2013). "Flexure on Dione: Investigating subsurface structure and thermal history". Icarus 223 (1): 418–422. doi:10.1016/j.icarus.2012.12.021. Retrieved 2015-05-29. 
  18. ^ Collins, G. C., ed. (2010). Testing Candidate Driving Forces for Faulting on Dione: Implications for Nonsynchronous Rotation and a Freezing Ocean. American Geophysical Union, Fall Meeting 2010, abstract #P24A-08. 
  19. ^ Phillips, C. B.; Hammond, N. P.; Roberts, J. H.; Nimmo, F. (2012). Subsurface Structure and Thermal History of Icy Satellites from Stereo Topography. American Geophysical Union, Fall Meeting 2012, abstract #P22B-03. 
  20. ^ "Cassini Finds Hints of Activity at Saturn Moon Dione". NASA News. 29 May 2013. Retrieved 2015-05-29. 
  21. ^ Jia-Rui Cook (May 29, 2013). "Cassini Finds Hints of Activity at Saturn Moon Dione". NASA. Retrieved October 1, 2013. 
  22. ^ "Cassini Prepares for Last Up-close Look at Hyperion". Jet Propulsion Laboratory. 28 May 2015. Retrieved 2015-05-29. 

External links

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