Methone was first discovered by the Cassini Imaging Team^[1][8][9] and given the temporary designation S/2004 S 1. Methone is also named Saturn XXXII (32). The Cassini spacecraft made two visits to Methone, and its closest approach was made on May 20, 2012 with a minimum distance of 1,900 km (1,181 mi) from it.

The name Methone was approved by the IAU Working Group on Planetary System Nomenclature on January 21, 2005.^[10] It was ratified at the IAU General Assembly in 2006. Methone (Greek Μεθώνη) was one of the Alkyonides, the seven beautiful daughters of the Giant Alkyoneus.

Methone's orbit is perturbed by a 14:15 mean-motion resonance with the much larger Mimas. This causes its osculating orbital elements to vary with an amplitude of about 20 km (12 mi) in semi-major axis, and 5° in longitude of its periapsis on a timescale of about 450 days. Its eccentricity also varies, albeit on different timescales, between 0.0011 and 0.0037, and its inclination between about 0.003° and 0.020°.^[4]

In May 2012, the Cassini spacecraft took its first close-up photographs of Methone, revealing a remarkably smooth, but non-spherical moonlet.^[11] The other arc-imbedded moonlets, Pallene and Aegaeon, are thought to be similar.^[12]

Methone's smoothness and excellent ellipsoidal fits suggest that it has developed an equipotential surface, and this may be composed largely of an icy fluff, a material that might be mobile enough to explain the moonlet's lack of craters. This material property causes Methone to take the shape of a triaxial ellipsoid, a type of ellipsoid in which all 3 of its principal axes are of different lengths. These differences reflect the balance between tidal forces exerted by Saturn and centrifugal forces from the moonlet's own rotation, as well as the moonlet's own force of gravity.^[13]

Methone's longest axis points towards Saturn, and is 1.6x longer than its polar axis. This elongation is caused by tidal forces, whereas the elongation of its intermediate-length axis (1.07x the length of the polar axis) is caused by the centrifugal force of Methone's rotation.^[13]

Methone's low-density regolith may respond to impacts in a way that smooths its surface more rapidly than on rigid moonlets such as Janus or Epimetheus. Movement of the regolith may also be facilitated by more "exotic" processes such as electrostatic effects.^[13]

Methone has two sharply defined albedo regions, with albedos of 0.61±0.06 and 0.7±0.03. The darker of these regions is centered on Methone's leading side, reminiscent of the thermal anomalies on the leading hemispheres of Mimas and Tethys,^[14] and it has been suggested that increased exposure to electrons from Saturn's magnetosphere is responsible. However, in those examples, the thermal anomalies coincide with a distinct UV/IR coloration, which in the case of Methone is either highly subdued or undetectable.^[13] Thus a physical, rather than compositional difference may be responsible. Possibilities include variations in regolith grain size, compaction, or particle microstructure.^[13]

Assuming that Methone is in hydrostatic equilibrium, i.e. that its elongated shape simply reflects the balance between the tidal force exerted by Saturn and Methone's gravity, its density can be estimated: 0.31+0.05
−0.03 g/cm³, among the lowest density values obtained or inferred for a Solar System body.^[13][12]

Material blasted off Methone by micrometeoroid impacts is believed to be the source of the Methone Ring Arc, a faint partial ring around Saturn co-orbital with Methone that was discovered in September 2006.^[15][16]

Citations edit

Sources edit

• "Cassini Imaging Science Team". Cassini Imaging Central Laboratory for Operations. Retrieved 2012-01-01.
• Battersby, S. (2013-05-17). "Saturn's egg moon Methone is made of fluff". www.newscientist.com. New Scientist. Retrieved 2013-05-21.
• Green, Daniel W. E. (August 16, 2004). "S/2004 S 1 and S/2004 S 2" (discovery). IAU Circular. 8389: 1. Bibcode:2004IAUC.8389....1P. Retrieved 2012-01-01.
• Green, Daniel W. E. (January 21, 2005). "S/2004 S 1 and S/2004 S 2" (naming the moon). IAU Circular. 8471. Retrieved 2012-01-01.
• Hedman, M. M.; Murray, C. D.; Cooper, N. J.; Tiscareno, M. S.; Beurle, K.; Evans, M. W.; Burns, J. A. (2008-11-25). "Three tenuous rings/arcs for three tiny moons". Icarus. 199 (2): 378–386. Bibcode:2009Icar..199..378H. doi:10.1016/j.icarus.2008.11.001. ISSN 0019-1035.
• "PIA06105: Cassini Uncovers New Moon". Photojournal. JPL/NASA. August 16, 2004. Retrieved 2012-01-01.
• Lakdawalla, E. (2012-05-21). "Methone, an egg in Saturn orbit?". www.planetary.org. The Planetary Society. Retrieved 2012-05-23.
• Porco, C. C.; Baker, E.; Barbara, J.; Beurle, K.; Brahic, A.; Burns, J. A.; Charnoz, S.; Cooper, N.; Dawson, D. D.; Del Genio, A. D.; Denk, T.; Dones, L.; Dyudina, U.; Evans, M. W.; Giese, B.; Grazier, K.; Helfenstein, P.; Ingersoll, A. P.; Jacobson, R. A.; Johnson, T. V.; McEwen, A.; Murray, C. D.; Neukum, G.; Owen, W. M.; Perry, J.; Roatsch, T.; Spitale, J.; Squyres, S.; Thomas, P.; Tiscareno, M. (February 25, 2005). "Cassini Imaging Science: Initial Results on Saturn's Rings and Small Satellites". Science. 307 (5713): 1226–1236. Bibcode:2005Sci...307.1226P. CiteSeerX 10.1.1.368.2642. doi:10.1126/science.1108056. PMID 15731439. S2CID 1058405.
• Schenk, P.; Hamilton, D. P.; Johnson, R. E.; McKinnon, W. B.; Paranicas, C.; Schmidt, J.; Showalter, M. R. (January 2011). "Plasma, plumes and rings: Saturn system dynamics as recorded in global color patterns on its midsize icy satellites". Icarus. 211 (1): 740–757. Bibcode:2011Icar..211..740S. doi:10.1016/j.icarus.2010.08.016.
• Carolyn Porco; et al. (2008-09-05). "More Ring Arcs for Saturn". Cassini Imaging Central Laboratory for Operations. Archived from the original on 2008-10-10. Retrieved 2008-09-05.
• Spitale, J. N.; Jacobson, R. A.; Porco, C. C.; Owen, W. M. Jr. (2006). "The orbits of Saturn's small satellites derived from combined historic and Cassini imaging observations". The Astronomical Journal. 132 (2): 692–710. Bibcode:2006AJ....132..692S. doi:10.1086/505206.
• Thomas, P. C. (July 2010). "Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission" (PDF). Icarus. 208 (1): 395–401. Bibcode:2010Icar..208..395T. doi:10.1016/j.icarus.2010.01.025.
• Thomas, P. C.; Burns, J. A.; Tiscareno, M. S.; Hedman, M. M.; et al. (2013). "Saturn's Mysterious Arc-Embedded Moons: Recycled Fluff?" (PDF). 44th Lunar and Planetary Science Conference. p. 1598. Retrieved 2013-05-21.
• Thomas, P. C.; Helfenstein, P. (July 2020). "The small inner satellites of Saturn: Shapes, structures and some implications". Icarus. 344: 20. Bibcode:2020Icar..34413355T. doi:10.1016/j.icarus.2019.06.016. S2CID 197474587. 113355.

• Methone Profile by NASA's Solar System Exploration
• IAU Working Group for Planetary System Nomenclature