Rhea (moon)

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Not to be confused with the asteroid named 577 Rhea.
Rhea
synchronous)
zero
Albedo0.949±0.003 (geometric) [9]
Surface temp. min mean max
Kelvin 53 K   99 K
10 [10]

Rhea (

ninth-largest moon in the Solar System, with a surface area that is comparable to the area of Australia. It is the smallest body in the Solar System for which precise measurements have confirmed a shape consistent with hydrostatic equilibrium.[11] It was discovered in 1672 by Giovanni Domenico Cassini
.

Discovery

Giovanni Domenico Cassini, discoverer of Rhea in 1672

Rhea was discovered by Giovanni Domenico Cassini on 23 December 1672.[1] It was the second moon of Saturn that Cassini discovered, and the third moon discovered around Saturn overall.[1]

Name

Rhea is named after the

Enceladus, Tethys, and Dione).[12][13]

Cassini named the four moons he discovered (Tethys, Dione, Rhea, and

Louis XIV.[1] Astronomers fell into the habit of referring to them and Titan as Saturn I through Saturn V.[1] Once Mimas and Enceladus were discovered, in 1789, the numbering scheme was extended to Saturn VII, and then to Saturn VIII with the discovery of Hyperion in 1848.[13]

Rhea was not named until 1847, when

Mimas and Enceladus) suggested in Results of Astronomical Observations made at the Cape of Good Hope that the names of the Titans, sisters and brothers of Kronos (Saturn, in Roman mythology), be used.[14][1]

Physical characteristics

Size, mass, and internal structure

Size comparison of Earth (right), the Moon (left top), and Rhea (left down)

Rhea is an icy body with a density of about 1.236 g/cm3. This low density indicates that it is made of ~25% rock (density ~3.25 g/cm3) and ~75% water ice (density ~0.93 g/cm3). Although Rhea is the ninth-largest moon, it is only the tenth-most massive moon. Indeed, Oberon, the second-largest moon of Uranus, has almost the same size, but is significantly denser than Rhea (1.63 vs 1.24) and thus more massive, although Rhea is slightly larger by volume. [b]

Before the Cassini-Huygens mission, it was assumed that Rhea had a rocky core.[15] However, measurements taken during a close flyby by the Cassini orbiter in 2005 cast this into doubt. In a paper published in 2007 it was claimed that the axial dimensionless moment of inertia coefficient was 0.4.[c][16] Such a value indicated that Rhea had an almost homogeneous interior (with some compression of ice in the center) while the existence of a rocky core would imply a moment of inertia of about 0.34.[15] In the same year another paper claimed the moment of inertia was about 0.37.[d] Rhea being either partially or fully differentiated would be consistent with the observations of the Cassini probe.[17] A year later yet another paper claimed that the moon may not be in hydrostatic equilibrium meaning that the moment of inertia cannot be determined from the gravity data alone.[18] In 2008 an author of the first paper tried to reconcile these three disparate results. He concluded that there is a systematic error in the Cassini radio Doppler data used in the analysis, but after restricting the analysis to a subset of data obtained closest to the moon, he arrived at his old result that Rhea was in hydrostatic equilibrium and had a moment of inertia of about 0.4, again implying a homogeneous interior.[8]

The

eutectic temperature for the water–ammonia system.[20] More recent indications are that Rhea has a homogeneous interior and hence that this ocean does not exist.[8]

Surface features

Main article: List of geological features on Rhea

Rhea's features resemble those of Dione, with dissimilar leading and trailing hemispheres, suggesting similar composition and histories. The temperature on Rhea is 99 K (−174 °C) in direct sunlight and between 73 K (−200 °C) and 53 K (−220 °C) in the shade.

Surface features on Rhea well defined due to the lighting.

Rhea has a rather typical heavily cratered surface,[21] with the exceptions of a few large Dione-type chasmata or fractures (wispy terrain) on the trailing hemisphere (the side facing away from the direction of motion along Rhea's orbit)[22] and a very faint "line" of material at Rhea's equator that may have been deposited by material deorbiting from its rings.[23] Rhea has two very large impact basins on its anti-Cronian hemisphere (facing away from Saturn), which are about 400 and 500 km across.[22] The more northerly and less degraded of the two, called Tirawa, is roughly comparable to the basin Odysseus on Tethys.[21] There is a 48 km-diameter impact crater at 112°W that is prominent because of an extended system of bright rays.[22] This crater, called Inktomi, is nicknamed "The Splat", and may be one of the youngest craters on the inner moons of Saturn.[22] No evidence of any endogenic activity has been discovered.[22]

Closeup showing two craters on Rhea's surface taken in 2013 by Cassini spacecraft.

Its surface can be divided into two geologically different areas based on crater density; the first area contains craters which are larger than 40 km in diameter, whereas the second area, in parts of the polar and equatorial regions, has only craters under that size. This suggests that a major resurfacing event occurred some time during its formation. The leading hemisphere is heavily cratered and uniformly bright. As on Callisto, the craters lack the high relief features seen on the Moon and Mercury. It has been theorized that these cratered plains are up to four billion years old on average.[24] On the trailing hemisphere there is a network of bright swaths on a dark background and few visible craters. It had been thought that these bright areas might be material ejected from ice volcanoes early in Rhea's history when its interior was still liquid. However, observations of Dione, which has an even darker trailing hemisphere and similar but more prominent bright streaks, show that the streaks are actually ice cliffs resulting from extensive fracturing of the moon's surface.[citation needed] The extensive dark areas are thought to be deposited tholins, which are a mix of complex organic compounds generated on the ice by pyrolysis and radiolysis of simple compounds containing carbon, nitrogen and hydrogen.[25]

The January 17, 2006 distant flyby by the

Cassini
spacecraft yielded images of the wispy hemisphere at better resolution and a lower Sun angle than previous observations. Images from this and subsequent flybys showed that Rhea's streaks in fact are tectonically formed ice cliffs (chasmata) similar to those of Dione.

Formation

The moons of Saturn are thought to have formed through

giant impacts between pre-existing moons, and Rhea and Iapetus are thought to have formed from part of the debris of these collisions.[26]

  • Image of the wispy hemisphere, showing ice cliffs - Powehiwehi (upper center); chasmata stretch from upper left to right center - Onokoro Catenae (lower right).
    Image of the wispy hemisphere, showing ice cliffs - Powehiwehi (upper center); chasmata stretch from upper left to right center - Onokoro Catenae (lower right).
  • View of Rhea's leading hemisphere with crater Inktomi and its prominent ray system just below center; impact basin Tirawa is at upper left
    View of Rhea's leading hemisphere with crater Inktomi and its prominent
    impact basin Tirawa
    is at upper left

Atmosphere

On November 27, 2010,

oxidation of the organics present in ice or to outgassing of the moon's interior.[27][28]

Possible ring system

Main article: Rings of Rhea

On March 6, 2008, NASA announced that Rhea may have a tenuous ring system. This would mark the first discovery of rings around a moon. The rings' existence was inferred by observed changes in the flow of electrons trapped by Saturn's magnetic field as Cassini passed by Rhea.[29][30][31] Dust and debris could extend out to Rhea's Hill sphere, but were thought to be denser nearer the moon, with three narrow rings of higher density. The case for a ring was strengthened by the subsequent finding of the presence of a set of small ultraviolet-bright spots distributed along Rhea's equator (interpreted as the impact points of deorbiting ring material).[32] However, when Cassini made targeted observations of the putative ring plane from several angles, no evidence of ring material was found, suggesting that another explanation for the earlier observations is needed.[33][34]

Exploration

The first images of Rhea were obtained by Voyager 1 & 2 spacecraft in 1980–1981.

There were five close targeted fly-bys by the Cassini orbiter: at a distance of 500 km on November 26, 2005, at a distance of 5,750 km on August 30, 2007, at a distance of 100 km on March 2, 2010, and at 69 km flyby on January 11, 2011[35] and a last flyby at 992 km on March 9, 2013.[36] Rhea has been also imaged many times from long to moderate distances by the orbiter.

See also

Notes

  1. ^ Calculated on the basis of other parameters.
  2. ^ The moons more massive than Rhea are: the Moon, the four Galilean moons, Titan, Triton, Titania, and Oberon. Oberon, Uranus's second-largest moon, has a radius that is ~0.4% smaller than Rhea's, but a density that is ~26% greater. See JPLSSD.
  3. ^ More precisely, 0.3911.[16]
  4. ^ More precisely, 0.3721.[17]

References

  1. ^ a b c d e f g Tillman, Nola Taylor (2016-06-29). "Rhea: Saturn's dirty snowball moon". space.com.
  2. doi:10.1029/EO063i006p00146
    . Retrieved Nov 30, 2022.
  3. ^ Moore et al. (1984) "The Geomorphology of Rhea", Proceedings of the fifteenth Lunar and Planetary Science, Part 2, p C-791–C-794
  4. ^ Natural Satellites Ephemeris Service Minor Planet Center
  5. ^ 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.
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  6. ^
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  7. doi:10.1029/2006GL028100
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  8. ^ a b c Anderson, John D. (July 2008). Rhea's Gravitational Field and Internal Structure. 37th COSPAR Scientific Assembly. Held 13–20 July 2008, in Montréal, Canada. p. 89.
    Bibcode:2008cosp...37...89A
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  9. ^ Verbiscer, A.; French, R.; Showalter, M.; Helfenstein, P. (9 February 2007). "Enceladus: Cosmic Graffiti Artist Caught in the Act". Science. 315 (5813): 815.
    S2CID 21932253
    .     (supporting online material, table S1)
  10. ^ Observatorio ARVAL (April 15, 2007). "Classic Satellites of the Solar System". Observatorio ARVAL. Retrieved 2011-12-17.
  11. ^ Thomas, P.C. (2010). "Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission" (PDF). Icarus. Archived from the original (PDF) on 2018-12-23.
  12. ^ "In Depth | Rhea". NASA Solar System Exploration. NASA Science. December 19, 2019. Retrieved January 7, 2020.
  13. ^ a b "Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. USGS Astrogeology. July 21, 2006. Retrieved January 7, 2020.
  14. ^ As reported by William Lassell, Monthly Notices of the Royal Astronomical Society, Vol. 8, No. 3, pp. 42–43 (January 14, 1848)
  15. ^ a b Anderson, J. D.; Rappaport, N. J.; Giampieri, G.; et al. (2003). "Gravity field and interior structure of Rhea".
    doi:10.1016/S0031-9201(03)00035-9
    .
  16. ^ a b Anderson, J. D.; Schubert, J. (2007). "Saturn's satellite Rhea is a homogeneous mix of rock and ice".
    doi:10.1029/2006GL028100
    .
  17. ^ a b Iess, L.; Rappaport, N.; Tortora, P.; Lunine, Jonathan I.; Armstrong, J.; Asmar, S.; Somenzi, L.; Zingoni, F. (2007). "Gravity field and interior of Rhea from Cassini data analysis". Icarus. 190 (2): 585.
    doi:10.1016/j.icarus.2007.03.027
    .
  18. ^ MacKenzie, R. A.; Iess, L.; Tortora, P.; Rappaport, N. J. (2008). "A non-hydrostatic Rhea". Geophysical Research Letters. 35 (5): L05204.
    hdl:11573/17051
    .
  19. ^ Thomas, P. C.; Burns, J. A.; Helfenstein, P.; Squyres, S.; Veverka, J.; Porco, C.; Turtle, E. P.; McEwen, A.; Denk, T.; Giesef, B.; Roatschf, T.; Johnsong, T. V.; Jacobsong, R. A. (October 2007). "Shapes of the saturnian icy satellites and their significance" (PDF). Icarus. 190 (2): 573–584.
    doi:10.1016/j.icarus.2007.03.012
    . Retrieved 15 December 2011.
  20. ^ Hussmann, Hauke; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects".
    doi:10.1016/j.icarus.2006.06.005
    .
  21. ^ a b Moore, Jeffrey M.; Schenk, Paul M.; Bruesch, Lindsey S.; Asphaug, Erik; McKinnon, William B. (October 2004). "Large impact features on middle-sized icy satellites" (PDF). Icarus. 171 (2): 421–443.
    doi:10.1016/j.icarus.2004.05.009
    .
  22. ^ a b c d e Wagner, R.J.; Neukum, G.; et al. (2008). "Geology of Saturn's Satellite Rhea on the Basis of the High-Resolution Images from the Targeted Flyby 049 on Aug. 30, 2007". Lunar and Planetary Science. XXXIX (1391): 1930.
    Bibcode:2008LPI....39.1930W
    .
  23. ^ Schenk, Paul M.; McKinnon, W. B. (2009). "Global Color Variations on Saturn's Icy Satellites, and New Evidence for Rhea's Ring". American Astronomical Society. 41: 3.03.
    Bibcode:2009DPS....41.0303S
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  24. ^ "Rhea - Overview | Planets - NASA Solar System Exploration". NASA Solar System Exploration. Archived from the original on 2016-02-14. Retrieved 2017-09-21.
  25. ^ A spectroscopic study of the surfaces of Saturn's large satellites: H2O ice, tholins, and minor constituents (PDF). Dale P. Cruikshank, Tobias. Owen, Cristina Dalle Ore, Thomas R. Geballe, Ted L. Roush, Catherine de Bergh, Scott A. Sandford, Francois Poulet, Gretchen K. Benedix, Joshua P. Emery. Icarus, 175, pages: 268–283, 2 March 2005.
  26. ^ "Giant impact scenario may explain the unusual moons of Saturn". Space Daily. 2012. Retrieved 2012-10-19.
  27. ^ "Cassini Finds Ethereal Atmosphere at Rhea". NASA. Archived from the original on September 16, 2011. Retrieved November 27, 2010.
  28. ^ Teolis, B. D.; Jones, G. H.; Miles, P. F.; Tokar, R. L.; Magee, B. A.; Waite, J. H.; Roussos, E.; Young, D. T.; Crary, F. J.; Coates, A. J.; Johnson, R. E.; Tseng, W. - L.; Baragiola, R. A. (2010). "Cassini Finds an Oxygen-Carbon Dioxide Atmosphere at Saturn's Icy Moon Rhea". Science. 330 (6012): 1813–1815.
    S2CID 206530211
    .
  29. ^ Saturn's Moon Rhea Also May Have Rings Archived 2012-10-22 at the Wayback Machine, NASA, June 3, 2006
  30. ^ Jones, G. H.; et al. (2008-03-07). "The Dust Halo of Saturn's Largest Icy Moon, Rhea". Science. 319 (5868): 1380–1384.
    S2CID 206509814
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  31. ^ Lakdawalla, E. (2008-03-06). "A Ringed Moon of Saturn? Cassini Discovers Possible Rings at Rhea". The Planetary Society web site.
    Planetary Society. Archived from the original on 2008-03-10. Retrieved 2008-03-09. {{cite web}}: External link in |work= (help
    )
  32. Planetary Society. Archived from the original on 2012-02-17. Retrieved 2009-10-06. {{cite web}}: External link in |work= (help
    )
  33. ^ Matthew S. Tiscareno; Joseph A. Burns; Jeffrey N. Cuzzi; Matthew M. Hedman (2010). "Cassini imaging search rules out rings around Rhea".
    S2CID 59458559
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  34. ^ Kerr, Richard A. (2010-06-25). "The Moon Rings That Never Were". ScienceNow. Archived from the original on 2010-07-01. Retrieved 2010-08-05.
  35. ^ Cook, Jia-Rui C. (13 January 2011). "Cassini Solstice Mission: Cassini Rocks Rhea Rendezvous". saturn.jpl.nasa.gov. NASA/JPL. Archived from the original on 17 January 2011. Retrieved 11 December 2011.
  36. ^ "NASA craft snaps last close-up photos of icy Saturn moon". saturn.jpl.nasa.gov. NASA/JPL. Retrieved 17 March 2013.

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