&sq=Facebook&lang=en&file=File:Io_highest_resolution_true_color.jpg) Enhanced color image of Io from the Galileo spacecraft, taken in 1999. | |||||||||
| Discovery | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| Discovered by | Galileo Galilei | ||||||||
| Discovery date | 8 January 1610[1] | ||||||||
| Designations | |||||||||
| Pronunciation | /ˈaɪ.oʊ/[2] or as Greco-Latin Īō (approximated as /ˈiː.oʊ/)[citation needed] | ||||||||
Named after | Ἰώ Īō | ||||||||
| Jupiter I | |||||||||
| Adjectives | Ionian /aɪˈoʊniən/[3][4] | ||||||||
| Orbital characteristics | |||||||||
| Periapsis | 420000 km (0.002808 AU) | ||||||||
| Apoapsis | 423400 km (0.002830 AU) | ||||||||
Mean orbit radius | 421700 km (0.002819 AU) | ||||||||
| Eccentricity | 0.0040313019 | ||||||||
| 1.769137786 d (152853.5047 s, 42.45930686 h) | |||||||||
Average orbital speed | 17.334 km/s | ||||||||
| Inclination | 0.05° (to Jupiter's equator) 2.213° (to the ecliptic) | ||||||||
| Satellite of | Jupiter | ||||||||
| Group | Galilean moon | ||||||||
| Physical characteristics | |||||||||
| Dimensions | 3,660.0 × 3,637.4 × 3,630.6 km[5] | ||||||||
| 1821.6±0.5 km (0.28592 Earths)[6] | |||||||||
| 41698064.7357 km2 (0.082 Earths) | |||||||||
| Volume | 2.5319064907×1010 km3 (0.023 Earths) | ||||||||
| Mass | (8.931938±0.000018)×1022 kg (0.015 Earths)[6] | ||||||||
Mean density | 3.528±0.006 g/cm3 (0.639 Earths)[6] | ||||||||
| 1.796502844 m/s2 (0.1831923077 g) | |||||||||
| 0.37824±0.00022[7] | |||||||||
| 2,558.3174910781 m/s | |||||||||
| synchronous | |||||||||
Equatorial rotation velocity | 271 km/h | ||||||||
North pole right ascension | 268.05°[8] | ||||||||
North pole declination | 64.50°[8] | ||||||||
| Albedo | 0.63±0.02[6] | ||||||||
| |||||||||
| 5.02 (opposition)[10] | |||||||||
| 1.2 arcseconds[11] | |||||||||
| Atmosphere | |||||||||
Surface pressure | 0.5 to 4 mPa (4.93×10−9 to 3.95×10−8 atm) | ||||||||
| Composition by volume | 90% sulfur dioxide | ||||||||
Io (/ˈaɪ.oʊ/), or Jupiter I, is the innermost and second-smallest of the four Galilean moons of the planet Jupiter. Slightly larger than Earth's moon, Io is the fourth-largest moon in the Solar System, has the highest density of any moon, the strongest surface gravity of any moon, and the lowest amount of water by atomic ratio of any known astronomical object in the Solar System. It was discovered in 1610 by Galileo Galilei and was named after the mythological character Io, a priestess of Hera who became one of Zeus's lovers.
With over 400 active volcanoes, Io is the most geologically active object in the Solar System.[12][13][14] This extreme geologic activity is the result of tidal heating from friction generated within Io's interior as it is pulled between Jupiter and the other Galilean moons—Europa, Ganymede and Callisto. Several volcanoes produce plumes of sulfur and sulfur dioxide that climb as high as 500 km (300 mi) above the surface. Io's surface is also dotted with more than 100 mountains that have been uplifted by extensive compression at the base of Io's silicate crust. Some of these peaks are taller than Mount Everest, the highest point on Earth's surface.[15] Unlike most moons in the outer Solar System, which are mostly composed of water ice, Io is primarily composed of silicate rock surrounding a molten iron or iron sulfide core. Most of Io's surface is composed of extensive plains with a frosty coating of sulfur and sulfur dioxide.
Io's volcanism is responsible for many of its unique features. Its volcanic plumes and lava flows produce large surface changes and paint the surface in various subtle shades of yellow, red, white, black, and green, largely due to allotropes and compounds of sulfur. Numerous extensive lava flows, several more than 500 km (300 mi) in length, also mark the surface. The materials produced by this volcanism make up Io's thin, patchy atmosphere, and they also greatly affect the nature and radiation levels of Jupiter's extensive magnetosphere. Io's volcanic ejecta also produce a large, intense plasma torus around Jupiter, creating a hostile radiation environment on and around the moon.[16]
Io played a significant role in the development of astronomy in the 17th and 18th centuries; discovered in January 1610 by Galileo Galilei, along with the other Galilean satellites, this discovery furthered the adoption of the Copernican model of the Solar System, the development of Kepler's laws of motion, and the first measurement of the speed of light. In 1979, the two Voyager spacecraft revealed Io to be a geologically active world, with numerous volcanic features, large mountains, and a young surface with no obvious impact craters. The Galileo spacecraft performed several close flybys in the 1990s and early 2000s, obtaining data about Io's interior structure and surface composition. These spacecraft also revealed the relationship between Io and Jupiter's magnetosphere and the existence of a belt of high-energy radiation centered on Io's orbit. Further observations have been made by Cassini–Huygens in 2000, New Horizons in 2007, and Juno since 2017, as well as from Earth-based telescopes and the Hubble Space Telescope.
- ^ Cite error: The named reference
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"Io". Merriam-Webster.com Dictionary. Merriam-Webster. - ^ Kieffer, S. W. (1982). "Dynamics and Thermodynamics of Volcanic Eruptions: Implications for the Plumes on Io". In Morrison, David; Matthews, Mildred Shapley (eds.). Satellites of Jupiter (PDF). Space science series. Tucson, Ariz: University of Arizona Press. ISBN 978-0-8165-0762-7.
- ^ Williams, D. J.; et al. (18 October 1996). "Electron Beams and Ion Composition Measured at Io and in Its Torus". Science. 274 (5286): 401–403. Bibcode:1996Sci...274..401W. doi:10.1126/science.274.5286.401. ISSN 0036-8075. PMID 8832885.
- ^ Thomas, P. C.; et al. (1998). "The Shape of Io from Galileo Limb Measurements". Icarus. 135 (1): 175–180. Bibcode:1998Icar..135..175T. doi:10.1006/icar.1998.5987.
- ^ a b c d Yeomans, Donald K. (13 July 2006). "Planetary Satellite Physical Parameters". JPL Solar System Dynamics.
- ^ Schubert, G.; Anderson, J. D.; Spohn, T.; McKinnon, W. B. (2004). "Interior composition, structure and dynamics of the Galilean satellites". In Bagenal, F.; Dowling, T. E.; McKinnon, W. B. (eds.). Jupiter : the planet, satellites, and magnetosphere. New York: Cambridge University Press. pp. 281–306. ISBN 978-0521035453. OCLC 54081598.
- ^ a b Archinal, B. A.; Acton, C. H.; A'Hearn, M. F.; Conrad, A.; Consolmagno, G. J.; Duxbury, T.; Hestroffer, D.; Hilton, J. L.; Kirk, R. L.; Klioner, S. A.; McCarthy, D.; Meech, K.; Oberst, J.; Ping, J.; Seidelmann, P. K. (2018). "Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2015". Celestial Mechanics and Dynamical Astronomy. 130 (3): 22. Bibcode:2018CeMDA.130...22A. doi:10.1007/s10569-017-9805-5. ISSN 0923-2958.
- ^ Rathbun, J. A.; Spencer, J.R.; Tamppari, L.K.; Martin, T.Z.; Barnard, L.; Travis, L.D. (2004). "Mapping of Io's thermal radiation by the Galileo photopolarimeter-radiometer (PPR) instrument". Icarus. 169 (1): 127–139. Bibcode:2004Icar..169..127R. doi:10.1016/j.icarus.2003.12.021.
- ^ "Classic Satellites of the Solar System". Observatorio ARVAL. Archived from the original on 9 July 2011. Retrieved 28 September 2007.
- ^ "Io". www.eso.org. 5 December 2001. Retrieved 21 May 2022.
- ^ Lopes, Rosaly MC (2007). "Io: The Volcanic Moon". In McFadden, Lucy-Ann Adams; Weissman, Paul R.; Johnson, Torrence V. (eds.). Encyclopedia of the solar system (2. ed.). Amsterdam Heidelberg: Academic Press. pp. 419–431. ISBN 978-0-12-088589-3.
- ^ Lopes, R. M. C.; et al. (2004). "Lava lakes on Io: Observations of Io's volcanic activity from Galileo NIMS during the 2001 fly-bys". Icarus. 169 (1): 140–174. Bibcode:2004Icar..169..140L. doi:10.1016/j.icarus.2003.11.013.
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- ^ "2000 February 29, SPS 1020 (Introduction to Space Sciences)". CSUFresno.edu. 29 February 2000. Archived from the original on 25 July 2008.