The dark spot just left of the center is the erupting volcano Prometheus. The whitish plains on either side of it are coated with volcanically deposited sulfur dioxide frost, whereas the yellower regions contain a higher proportion of sulfur.
Enhanced color image of Io from the Galileo spacecraft, taken in 1999.
Discovered byGalileo Galilei
Discovery date8 January 1610[1]
Pronunciation/ˈ./[2] or as Greco-Latin Īō (approximated as /ˈ./)[citation needed]
Named after
Ἰώ Īō
Jupiter I
AdjectivesIonian /ˈniən/[3][4]
Orbital characteristics
Periapsis420000 km (0.002808 AU)
Apoapsis423400 km (0.002830 AU)
Mean orbit radius
421700 km (0.002819 AU)
1.769137786 d (152853.5047 s, 42.45930686 h)
17.334 km/s
Inclination0.05° (to Jupiter's equator)
2.213° (to the ecliptic)
Satellite ofJupiter
GroupGalilean moon
Physical characteristics
Dimensions3,660.0 × 3,637.4 × 3,630.6 km[5]
Mean radius
1821.6±0.5 km (0.28592 Earths)[6]
41698064.7357 km2 (0.082 Earths)
Volume2.5319064907×1010 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)
2,558.3174910781 m/s
Equatorial rotation velocity
271 km/h
Surface temp. min mean max
Surface 90 K 110 K 130 K[8]
5.02 (opposition)[9]
1.2 arcseconds[10]
Surface pressure
0.5 to 4 mPa (4.93×10−9 to 3.95×10−8 atm)
Composition by volume90% sulfur dioxide

Io (/ˈ./), 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.[11][12][13] 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.[14] 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; Io receives about 3,600 rem (36 Sv) of ionizing radiation per day.[15]

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.


Main article: Galilean moons § Names

See also: List of regions on Io, List of volcanic features on Io, and List of mountains on Io

Size comparison between Io (lower left), the Moon (upper left) and Earth

Although Simon Marius is not credited with the sole discovery of the Galilean satellites, his names for the moons were adopted.[16] In his 1614 publication Mundus Iovialis anno M.DC.IX Detectus Ope Perspicilli Belgici, he proposed several alternative names for the innermost of the large moons of Jupiter, including "The Mercury of Jupiter" and "The First of the Jovian Planets".[16][17] Based on a suggestion from Johannes Kepler in October 1613, he also devised a naming scheme whereby each moon was named for a lover of the Greek god Zeus or his Roman equivalent, Jupiter. He named the innermost large moon of Jupiter after the Greek Io:[18][16]

Jupiter is much blamed by the poets on account of his irregular loves. Three maidens are especially mentioned as having been clandestinely courted by Jupiter with success. Io, daughter of the River Inachus, Callisto of Lycaon, Europa of Agenor. Then there was Ganymede, the handsome son of King Tros, whom Jupiter, having taken the form of an eagle, transported to heaven on his back, as poets fabulously tell... I think, therefore, that I shall not have done amiss if the First is called by me Io, the Second Europa, the Third, on account of its majesty of light, Ganymede, the Fourth Callisto...[16]

Marius's names were not widely adopted until centuries later (mid-20th century).[19] In much of the earlier astronomical literature, Io was generally referred to by its Roman numeral designation (a system introduced by Galileo) as "Jupiter I",[20] or as "the first satellite of Jupiter".[21][22]

The customary English pronunciation of the name is /ˈ/,[23] though sometimes people attempt a more 'authentic' pronunciation, /ˈ/.[24] The name has two competing stems in Latin: Īō and (rarely) Īōn.[25] The latter is the basis of the English adjectival form, Ionian.[26][27][28]

Features on Io are named after characters and places from the Io myth, as well as deities of fire, volcanoes, the Sun, and thunder from various myths, and characters and places from Dante's Inferno: names appropriate to the volcanic nature of the surface.[29] Since the surface was first seen up close by Voyager 1, the International Astronomical Union has approved 249 names for Io's volcanoes, mountains, plateaus, and large albedo features. The approved feature categories used for Io for different types of volcanic features include patera ('saucer'; volcanic depression), fluctus ('flow'; lava flow), vallis ('valley'; lava channel), and active eruptive center (location where plume activity was the first sign of volcanic activity at a particular volcano). Named mountains, plateaus, layered terrain, and shield volcanoes include the terms mons, mensa ('table'), planum, and tholus ('rotunda'), respectively.[29] Named, bright albedo regions use the term regio. Examples of named features are Prometheus, Pan Mensa, Tvashtar Paterae, and Tsũi Goab Fluctus.[30]

Observational history

Main article: Exploration of Io

Galileo Galilei, the discoverer of Io

The first reported observation of Io was made by Galileo Galilei on 7 January 1610 using a 20x-power, refracting telescope at the University of Padua. However, in that observation, Galileo could not separate Io and Europa due to the low power of his telescope, so the two were recorded as a single point of light. Io and Europa were seen for the first time as separate bodies during Galileo's observations of the Jovian system the following day, 8 January 1610 (used as the discovery date for Io by the IAU).[1] The discovery of Io and the other Galilean satellites of Jupiter was published in Galileo's Sidereus Nuncius in March 1610.[31] In his Mundus Jovialis, published in 1614, Simon Marius claimed to have discovered Io and the other moons of Jupiter in 1609, one week before Galileo's discovery. Galileo doubted this claim and dismissed the work of Marius as plagiarism. Regardless, Marius's first recorded observation came from 29 December 1609 in the Julian calendar, which equates to 8 January 1610 in the Gregorian calendar, which Galileo used.[32] Given that Galileo published his work before Marius, Galileo is credited with the discovery.[33]

For the next two and a half centuries, Io remained an unresolved, 5th-magnitude point of light in astronomers' telescopes. During the 17th century, Io and the other Galilean satellites served a variety of purposes, including early methods to determine longitude,[34] validating Kepler's third law of planetary motion, and determining the time required for light to travel between Jupiter and Earth.[31] Based on ephemerides produced by astronomer Giovanni Cassini and others, Pierre-Simon Laplace created a mathematical theory to explain the resonant orbits of Io, Europa, and Ganymede.[31] This resonance was later found to have a profound effect on the geologies of the three moons.[35]

Improved telescope technology in the late 19th and 20th centuries allowed astronomers to resolve (that is, see as distinct objects) large-scale surface features on Io. In the 1890s, Edward E. Barnard was the first to observe variations in Io's brightness between its equatorial and polar regions, correctly determining that this was due to differences in color and albedo between the two regions and not due to Io being egg-shaped, as proposed at the time by fellow astronomer William Pickering, or two separate objects, as initially proposed by Barnard.[21][22][36] Later telescopic observations confirmed Io's distinct reddish-brown polar regions and yellow-white equatorial band.[37]

Telescopic observations in the mid-20th century began to hint at Io's unusual nature. Spectroscopic observations suggested that Io's surface was devoid of water ice (a substance found to be plentiful on the other Galilean satellites).[38] The same observations suggested a surface dominated by evaporates composed of sodium salts and sulfur.[39] Radiotelescopic observations revealed Io's influence on the Jovian magnetosphere, as demonstrated by decametric wavelength bursts tied to the orbital period of Io.[40]


The first spacecraft to pass by Io were the Pioneer 10 and 11 probes on 3 December 1973 and 2 December 1974, respectively.[41] Radio tracking provided an improved estimate of Io's mass, which, along with the best available information of its size, suggested it had the highest density of the Galilean satellites, and was composed primarily of silicate rock rather than water ice.[42] The Pioneers also revealed the presence of a thin atmosphere and intense radiation belts near the orbit of Io. The camera on board Pioneer 11 took the only good image of the moon obtained by either spacecraft, showing its north polar region and its yellow tint.[43] Close-up images were planned during Pioneer 10's encounter, but those were lost because of the high-radiation environment.[41]


Voyager 1 mosaic covering Io's south polar region. This includes two of Io's ten highest peaks, the Euboea Montes at upper extreme left and Haemus Mons at bottom.

When the twin probes Voyager 1 and Voyager 2 passed by Io in 1979, their more advanced imaging systems allowed for far more detailed images. Voyager 1 flew past Io on 5 March 1979 from a distance of 20,600 km (12,800 mi).[44] The images returned during the approach revealed a strange, multi-colored landscape devoid of impact craters.[45][46] The highest-resolution images showed a relatively young surface punctuated by oddly shaped pits, mountains taller than Mount Everest, and features resembling volcanic lava flows.[45][47]

Shortly after the encounter, Voyager navigation engineer Linda A. Morabito noticed a plume emanating from the surface in one of the images.[48] Analysis of other Voyager 1 images showed nine such plumes scattered across the surface, proving that Io was volcanically active.[49] This conclusion was predicted in a paper published shortly before the Voyager 1 encounter by Stan Peale, Patrick Cassen, and R. T. Reynolds. The authors calculated that Io's interior must experience significant tidal heating caused by its orbital resonance with Europa and Ganymede (see the "Tidal heating" section for a more detailed explanation of the process).[50] Data from this flyby showed that the surface of Io is dominated by sulfur and sulfur dioxide frosts. These compounds also dominate its thin atmosphere and the torus of plasma centered on Io's orbit (also discovered by Voyager).[51][52][53]

Voyager 2 passed Io on 9 July 1979 at a distance of 1,130,000 km (700,000 mi). Though it did not approach nearly as close as Voyager 1, comparisons between images taken by the two spacecraft showed several surface changes that had occurred in the four months between the encounters. In addition, observations of Io as a crescent as Voyager 2 departed the Jovian system revealed that seven of the nine plumes observed in March were still active in July 1979, with only the volcano Pele shutting down between flybys.[54]


Enhanced-color Galileo image showing a dark spot (just lower-left of center, interrupting the red ring of short-chain sulfur allotropes deposited by Pele) produced by a major eruption at Pillan Patera in 1997

The Galileo spacecraft arrived at Jupiter in 1995 after a six-year journey from Earth to follow up on the discoveries of the two Voyager probes and the ground-based observations made in the intervening years. Io's location within one of Jupiter's most intense radiation belts precluded a prolonged close flyby, but Galileo did pass close by shortly before entering orbit for its two-year, primary mission studying the Jovian system. Although no images were taken during the close flyby on 7 December 1995, the encounter did yield significant results, such as the discovery of a large iron core, similar to that found on the rocky planets of the inner Solar System.[55]

Despite the lack of close-up imaging and mechanical problems that greatly restricted the amount of data returned, several significant discoveries were made during Galileo's primary mission. Galileo observed the effects of a major eruption at Pillan Patera and confirmed that volcanic eruptions are composed of silicate magmas with magnesium-rich mafic and ultramafic compositions.[56] Distant imaging of Io was acquired for almost every orbit during the primary mission, revealing large numbers of active volcanoes (both thermal emission from cooling magma on the surface and volcanic plumes), numerous mountains with widely varying morphologies, and several surface changes that had taken place both between the Voyager and Galileo eras and between Galileo orbits.[57]

The Galileo mission was twice extended, in 1997 and 2000. During these extended missions, the probe flew by Io three times in late 1999 and early 2000, and three times in late 2001 and early 2002. Observations during these encounters revealed the geologic processes occurring at Io's volcanoes and mountains, excluded the presence of a magnetic field, and demonstrated the extent of volcanic activity.[57]


The Cassini-Huygens mission's view of Io and Jupiter on January 1, 2001

In December 2000, the Cassini spacecraft had a distant and brief encounter with the Jovian system en route to Saturn, allowing for joint observations with Galileo. These observations revealed a new plume at Tvashtar Paterae and provided insights into Io's aurorae.[58]

New Horizons

The New Horizons spacecraft, en route to Pluto and the Kuiper belt, flew by the Jovian system and Io on 28 February 2007. During the encounter, numerous distant observations of Io were obtained. These included images of a large plume at Tvashtar, providing the first detailed observations of the largest class of Ionian volcanic plume since observations of Pele's plume in 1979.[59] New Horizons also captured images of a volcano near Girru Patera in the early stages of an eruption, and several volcanic eruptions that have occurred since Galileo.[59]


Global image of Jupiter's moon Io acquired by Juno's JunoCam camera on December 30, 2023

The Juno spacecraft was launched in 2011 and entered orbit around Jupiter on July 5, 2016. Juno's mission is primarily focused on improving our understanding of Jupiter's interior, magnetic field, aurorae, and polar atmosphere.[60] Juno's 54-day orbit is highly inclined and highly eccentric in order to better characterize Jupiter's polar regions and to limit its exposure to the planet's harsh inner radiation belts, limiting close encounters with Jupiter's moons. The closest approach to Io during the initial, prime mission occurred in February 2020 at a distance of 195,000 kilomters.[61] Juno's extended mission, begun in June 2021, allowed for closer encounters with Jupiter's Galilean satellites due to Juno's orbital precession.[62] After a series of increasingly closer encounters with Io in 2022 and 2023, Juno performed a pair of close flybys on December 30, 2023,[63] and February 3, 2024,[64] both with altitudes of 1,500 kilometers. The primary goal of these encounters were to improve our understanding of Io's gravity field using doppler tracking and to image Io's surface to look for surface changes since Io was last seen up-close in 2007.[65]

During several orbits, Juno has observed Io from a distance using JunoCAM, a wide-angle, visible-light camera, to look for volcanic plumes and JIRAM, a near-infrared spectrometer and imager, to monitor thermal emission from Io's volcanoes.[66][61] JIRAM near-infrared spectroscopy has so far allowed for the coarse mapping of sulfur dioxide frost across Io's surface as well as mapping minor surface components weakly absorbing sunlight at 2.1 and 2.65 μm.[67]

Future missions

There are two forthcoming missions planned for the Jovian system. The Jupiter Icy Moon Explorer (JUICE) is a planned European Space Agency mission to the Jovian system that is intended to end up in Ganymede orbit.[68] JUICE launched in April 2023, with arrival at Jupiter planned for July 2031.[69][70] JUICE will not fly by Io, but it will use its instruments, such as a narrow-angle camera, to monitor Io's volcanic activity and measure its surface composition during the two-year Jupiter-tour phase of the mission prior to Ganymede orbit insertion. Europa Clipper is a planned NASA mission to the Jovian system focused on Jupiter's moon Europa. Like JUICE, Europa Clipper will not perform any flybys of Io, but distant volcano monitoring is likely. Europa Clipper has a planned launch in 2024 with an arrival at Jupiter in 2030.[71]

The Io Volcano Observer (IVO) was a proposal to NASA for a low-cost, Discovery-class mission selected for a Phase A study along with three other missions in 2020. IVO would launch in January 2029 and perform ten flybys of Io while in orbit around Jupiter beginning in the early 2030s.[72][73] However, the Venus missions DAVINCI+ and VERITAS were selected in favor of those.[74]

Orbit and rotation

Animation of the Laplace resonance of Io, Europa and Ganymede (conjunctions are highlighted by color changes)

See also: Tidal heating

Io orbits Jupiter at a distance of 421,700 km (262,000 mi) from Jupiter's center and 350,000 km (217,000 mi) from its cloudtops. It is the innermost of the Galilean satellites of Jupiter, its orbit lying between those of Thebe and Europa. Including Jupiter's inner satellites, Io is the fifth moon out from Jupiter. It takes Io about 42.5 hours (1.77 days) to complete one orbit around Jupiter (fast enough for its motion to be observed over a single night of observation). Io is in a 2:1 mean-motion orbital resonance with Europa and a 4:1 mean-motion orbital resonance with Ganymede, completing two orbits of Jupiter for every one orbit completed by Europa, and four orbits for every one completed by Ganymede. This resonance helps maintain Io's orbital eccentricity (0.0041), which in turn provides the primary heating source for its geologic activity.[50] Without this forced eccentricity, Io's orbit would circularize through tidal dissipation, leading to a less geologically active world.[50]

Like the other Galilean satellites and the Moon, Io rotates synchronously with its orbital period, keeping one face nearly pointed toward Jupiter. This synchrony provides the definition for Io's longitude system. Io's prime meridian intersects the equator at the sub-Jovian point. The side of Io that always faces Jupiter is known as the subjovian hemisphere, whereas the side that always faces away is known as the antijovian hemisphere. The side of Io that always faces in the direction that Io travels in its orbit is known as the leading hemisphere, whereas the side that always faces in the opposite direction is known as the trailing hemisphere.[75]

From the surface of Io, Jupiter would subtend an arc of 19.5°, making Jupiter appear 39 times the apparent diameter of Earth's Moon.[citation needed]

Interaction with Jupiter's magnetosphere

Schematic of Jupiter's magnetosphere and the components influenced by Io (near the center of the image): the plasma torus (in red), the neutral cloud (in yellow), the flux tube (in green), and magnetic field lines (in blue).[76]

Io plays a significant role in shaping Jupiter's magnetic field, acting as an electric generator that can develop 400,000 volts across itself and create an electric current of 3 million amperes, releasing ions that give Jupiter a magnetic field inflated to more than twice the size it would otherwise have.[77] The magnetosphere of Jupiter sweeps up gases and dust from Io's thin atmosphere at a rate of 1 tonne per second.[78] This material is mostly composed of ionized and atomic sulfur, oxygen and chlorine; atomic sodium and potassium; molecular sulfur dioxide and sulfur; and sodium chloride dust.[78][79] These materials originate from Io's volcanic activity, with the material that escapes to Jupiter's magnetic field and into interplanetary space coming directly from Io's atmosphere. These materials, depending on their ionized state and composition, end up in various neutral (non-ionized) clouds and radiation belts in Jupiter's magnetosphere and, in some cases, are eventually ejected from the Jovian system.[80]

The Jupiter - Io System and Interaction
(artwork; 15 July 2021)

Surrounding Io (at a distance of up to six Io radii from its surface) is a cloud of neutral sulfur, oxygen, sodium, and potassium atoms. These particles originate in Io's upper atmosphere and are excited by collisions with ions in the plasma torus (discussed below) and by other processes into filling Io's Hill sphere, which is the region where Io's gravity is dominant over Jupiter's. Some of this material escapes Io's gravitational pull and goes into orbit around Jupiter. Over a 20-hour period, these particles spread out from Io to form a banana-shaped, neutral cloud that can reach as far as six Jovian radii from Io, either inside Io's orbit and ahead of it or outside Io's orbit and behind it.[78] The collision process that excites these particles also occasionally provides sodium ions in the plasma torus with an electron, removing those new "fast" neutrals from the torus. These particles retain their velocity (70 km/s, compared to the 17 km/s orbital velocity at Io), and are thus ejected in jets leading away from Io.[81]

Io orbits within a belt of intense radiation known as the Io plasma torus. The plasma in this doughnut-shaped ring of ionized sulfur, oxygen, sodium, and chlorine originates when neutral atoms in the "cloud" surrounding Io are ionized and carried along by the Jovian magnetosphere.[78] Unlike the particles in the neutral cloud, these particles co-rotate with Jupiter's magnetosphere, revolving around Jupiter at 74 km/s. Like the rest of Jupiter's magnetic field, the plasma torus is tilted with respect to Jupiter's equator (and Io's orbital plane), so that Io is at times below and at other times above the core of the plasma torus. As noted above, these ions' higher velocity and energy levels are partly responsible for the removal of neutral atoms and molecules from Io's atmosphere and more extended neutral clouds. The torus is composed of three sections: an outer, "warm" torus that resides just outside Io's orbit; a vertically extended region known as the "ribbon", composed of the neutral source region and cooling plasma, located at around Io's distance from Jupiter; and an inner, "cold" torus, composed of particles that are slowly spiraling in toward Jupiter.[78] After residing an average of 40 days in the torus, particles in the "warm" torus escape and are partially responsible for Jupiter's unusually large magnetosphere, their outward pressure inflating it from within.[82] Particles from Io, detected as variations in magnetospheric plasma, have been detected far into the long magnetotail by New Horizons. To study similar variations within the plasma torus, researchers measured the ultraviolet light it emits. Although such variations have not been definitively linked to variations in Io's volcanic activity (the ultimate source for material in the plasma torus), this link has been established in the neutral sodium cloud.[83]

During an encounter with Jupiter in 1992, the Ulysses spacecraft detected a stream of dust-sized particles being ejected from the Jovian system.[84] The dust in these discrete streams travels away from Jupiter at speeds upwards of several hundred kilometers per second, has an average particle size of 10 μm, and consists primarily of sodium chloride.[79][85] Dust measurements by Galileo showed that these dust streams originated on Io, but exactly how these form, whether from Io's volcanic activity or material removed from the surface, is unknown.[86]

Jupiter's magnetic field, which Io crosses, couples Io's atmosphere and neutral cloud to Jupiter's polar upper atmosphere by generating an electric current known as the Io flux tube.[78] This current produces an auroral glow in Jupiter's polar regions known as the Io footprint, as well as aurorae in Io's atmosphere. Particles from this auroral interaction darken the Jovian polar regions at visible wavelengths. The location of Io and its auroral footprint with respect to Earth and Jupiter has a strong influence on Jovian radio emissions from our vantage point: when Io is visible, radio signals from Jupiter increase considerably.[40][78] The Juno mission, currently in orbit around Jupiter, should help shed light on these processes. The Jovian magnetic field lines that do get past Io's ionosphere also induce an electric current, which in turn creates an induced magnetic field within Io's interior. Io's induced magnetic field is thought to be generated within a partially molten, silicate magma ocean 50 kilometers beneath Io's surface.[87] Similar induced fields were found at the other Galilean satellites by Galileo, possibly generated within liquid water oceans in the interiors of those moons.[88]


Io is slightly larger than Earth's Moon. It has a mean radius of 1,821.3 km (1,131.7 mi) (about 5% greater than the Moon's) and a mass of 8.9319×1022 kg (about 21% greater than the Moon's). It is a slight ellipsoid in shape, with its longest axis directed toward Jupiter. Among the Galilean satellites, in both mass and volume, Io ranks behind Ganymede and Callisto but ahead of Europa.[89]


Model of the possible interior composition of Io with various features labelled.

Composed primarily of silicate rock and iron, Io and Europa are closer in bulk composition to terrestrial planets than to other satellites in the outer Solar System, which are mostly composed of a mix of water ice and silicates. Io has a density of 3.5275 g/cm3, the highest of any regular moon in the Solar System; significantly higher than the other Galilean satellites (Ganymede and Callisto in particular, whose densities are around 1.9 g/cm3) and slightly higher (~5.5%) than the Moon's 3.344 g/cm3 and Europa's 2.989 g/cm3.[7] Models based on the Voyager and Galileo measurements of Io's mass, radius, and quadrupole gravitational coefficients (numerical values related to how mass is distributed within an object) suggest that its interior is differentiated between a silicate-rich crust and mantle and an iron- or iron-sulfide-rich core.[55] Io's metallic core makes up approximately 20% of its mass.[90] Depending on the amount of sulfur in the core, the core has a radius between 350 and 650 km (220–400 mi) if it is composed almost entirely of iron, or between 550 and 900 km (340–560 mi) for a core consisting of a mix of iron and sulfur. Galileo's magnetometer failed to detect an internal, intrinsic magnetic field at Io, suggesting that the core is not convecting.[91]

Modeling of Io's interior composition suggests that the mantle is composed of at least 75% of the magnesium-rich mineral forsterite, and has a bulk composition similar to that of L-chondrite and LL-chondrite meteorites, with higher iron content (compared to silicon) than the Moon or Earth, but lower than Mars.[92][93] To support the heat flow observed on Io, 10–20% of Io's mantle may be molten, though regions where high-temperature volcanism has been observed may have higher melt fractions.[94] However, re-analysis of Galileo magnetometer data in 2009 revealed the presence of an induced magnetic field at Io, requiring a magma ocean 50 km (31 mi) below the surface.[87] Further analysis published in 2011 provided direct evidence of such an ocean.[95] This layer is estimated to be 50 km thick and to make up about 10% of Io's mantle. It is estimated that the temperature in the magma ocean reaches 1,200 °C. It is not known if the 10–20% partial melting percentage for Io's mantle is consistent with the requirement for a significant amount of molten silicates in this possible magma ocean.[96] The lithosphere of Io, composed of basalt and sulfur deposited by Io's extensive volcanism, is at least 12 km (7.5 mi) thick, and likely less than 40 km (25 mi) thick.[90][97]

Tidal heating

Main article: Tidal heating of Io

Unlike Earth and the Moon, Io's main source of internal heat comes from tidal dissipation rather than radioactive isotope decay, the result of Io's orbital resonance with Europa and Ganymede.[50] Such heating is dependent on Io's distance from Jupiter, its orbital eccentricity, the composition of its interior, and its physical state.[94] Its Laplace resonance with Europa and Ganymede maintains Io's eccentricity and prevents tidal dissipation within Io from circularizing its orbit. The resonant orbit also helps to maintain Io's distance from Jupiter; otherwise tides raised on Jupiter would cause Io to slowly spiral outward from its parent planet.[98] The tidal forces experienced by Io are about 20,000 times stronger than the tidal forces Earth experiences due to the Moon, and the vertical differences in its tidal bulge, between the times Io is at periapsis and apoapsis in its orbit, could be as much as 100 m (330 ft).[99] The friction or tidal dissipation produced in Io's interior due to this varying tidal pull, which, without the resonant orbit, would have gone into circularizing Io's orbit instead, creates significant tidal heating within Io's interior, melting a significant amount of Io's mantle and core. The amount of energy produced is up to 200 times greater than that produced solely from radioactive decay.[11] This heat is released in the form of volcanic activity, generating its observed high heat flow (global total: 0.6 to 1.6×1014 W).[94] Models of its orbit suggest that the amount of tidal heating within Io changes with time; however, the current amount of tidal dissipation is consistent with the observed heat flow.[94][100] Models of tidal heating and convection have not found consistent planetary viscosity profiles that simultaneously match tidal energy dissipation and mantle convection of heat to the surface.[100][101]

Although there is general agreement that the origin of the heat as manifested in Io's many volcanoes is tidal heating from the pull of gravity from Jupiter and its moon Europa, the volcanoes are not in the positions predicted with tidal heating. They are shifted 30 to 60 degrees to the east.[102] A study published by Tyler et al. (2015) suggests that this eastern shift may be caused by an ocean of molten rock under the surface. The movement of this magma would generate extra heat through friction due to its viscosity. The study's authors believe that this subsurface ocean is a mixture of molten and solid rock.[103]

Other moons in the Solar System are also tidally heated, and they too may generate additional heat through the friction of subsurface magma or water oceans. This ability to generate heat in a subsurface ocean increases the chance of life on bodies like Europa and Enceladus.[104][105]


Io's surface map

Based on their experience with the ancient surfaces of the Moon, Mars, and Mercury, scientists expected to see numerous impact craters in Voyager 1's first images of Io. The density of impact craters across Io's surface would have given clues to Io's age. However, they were surprised to discover that the surface was almost completely lacking in impact craters, but was instead covered in smooth plains dotted with tall mountains, pits of various shapes and sizes, and volcanic lava flows.[45] Compared to most worlds observed to that point, Io's surface was covered in a variety of colorful materials (leading Io to be compared to a rotten orange or to pizza) from various sulfurous compounds.[106][107] The lack of impact craters indicated that Io's surface is geologically young, like the terrestrial surface; volcanic materials continuously bury craters as they are produced. This result was spectacularly confirmed as at least nine active volcanoes were observed by Voyager 1.[49]

Surface composition

Io's colorful appearance is the result of materials deposited by its extensive volcanism, including silicates (such as orthopyroxene), sulfur, and sulfur dioxide.[108] Sulfur dioxide frost is ubiquitous across the surface of Io, forming large regions covered in white or grey materials. Sulfur is also seen in many places across Io, forming yellow to yellow-green regions. Sulfur deposited in the mid-latitude and polar regions is often damaged by radiation, breaking up the normally stable cyclic 8-chain sulfur. This radiation damage produces Io's red-brown polar regions.[21]

Geological map of Io

Explosive volcanism, often taking the form of umbrella-shaped plumes, paints the surface with sulfurous and silicate materials. Plume deposits on Io are often colored red or white depending on the amount of sulfur and sulfur dioxide in the plume. Generally, plumes formed at volcanic vents from degassing lava contain a greater amount of S2, producing a red "fan" deposit, or in extreme cases, large (often reaching beyond 450 km or 280 mi from the central vent) red rings.[109] A prominent example of a red-ring plume deposit is located at Pele. These red deposits consist primarily of sulfur (generally 3- and 4-chain molecular sulfur), sulfur dioxide, and perhaps sulfuryl chloride.[108] Plumes formed at the margins of silicate lava flows (through the interaction of lava and pre-existing deposits of sulfur and sulfur dioxide) produce white or gray deposits.[110]

Compositional mapping and Io's high density suggest that Io contains little to no water, though small pockets of water ice or hydrated minerals have been tentatively identified, most notably on the northwest flank of the mountain Gish Bar Mons.[111] Io has the least amount of water of any known body in the Solar System.[112] This lack of water is likely due to Jupiter being hot enough early in the evolution of the Solar System to drive off volatile materials like water in the vicinity of Io, but not hot enough to do so farther out.[113]


Main article: Volcanism on Io

See also: List of volcanic features on Io

Active lava flows in volcanic region Tvashtar Paterae (blank region represents saturated areas in the original data). Images taken by Galileo in November 1999 and February 2000.

The tidal heating produced by Io's forced orbital eccentricity has made it the most volcanically active world in the Solar System, with hundreds of volcanic centers and extensive lava flows.[13] During a major eruption, lava flows tens or even hundreds of kilometers long can be produced, consisting mostly of basalt silicate lavas with either mafic or ultramafic (magnesium-rich) compositions. As a by-product of this activity, sulfur, sulfur dioxide gas and silicate pyroclastic material (like ash) are blown up to 200 km (120 mi) into space, producing large, umbrella-shaped plumes, painting the surrounding terrain in red, black, and white, and providing material for Io's patchy atmosphere and Jupiter's extensive magnetosphere.[114][80]

Loki Patera on moon Io (artist's concept; animation; 0:18)[115]

Io's surface is dotted with volcanic depressions known as paterae which generally have flat floors bounded by steep walls.[116] These features resemble terrestrial calderas, but it is unknown if they are produced through collapse over an emptied lava chamber like their terrestrial cousins. One hypothesis suggests that these features are produced through the exhumation of volcanic sills, and the overlying material is either blasted out or integrated into the sill.[117] Examples of paterae in various stages of exhumation have been mapped using Galileo images of the Chaac-Camaxtli region.[118] Unlike similar features on Earth and Mars, these depressions generally do not lie at the peak of shield volcanoes and are normally larger, with an average diameter of 41 km (25 mi), the largest being Loki Patera at 202 km (126 mi).[116] Loki is also consistently the strongest volcano on Io, contributing on average 25% of Io's global heat output.[119] Whatever the formation mechanism, the morphology and distribution of many paterae suggest that these features are structurally controlled, with at least half bounded by faults or mountains.[116] These features are often the site of volcanic eruptions, either from lava flows spreading across the floors of the paterae, as at an eruption at Gish Bar Patera in 2001, or in the form of a lava lake.[12][120] Lava lakes on Io either have a continuously overturning lava crust, such as at Pele, or an episodically overturning crust, such as at Loki.[121][122]

Jupiter moon Io volcanic activity
(12/14/2022/left and 03/01/2023)

Lava flows represent another major volcanic terrain on Io. Magma erupts onto the surface from vents on the floor of paterae or on the plains from fissures, producing inflated, compound lava flows similar to those seen at Kilauea in Hawaii. Images from the Galileo spacecraft revealed that many of Io's major lava flows, like those at Prometheus and Amirani, are produced by the build-up of small breakouts of lava flows on top of older flows.[123] Larger outbreaks of lava have also been observed on Io. For example, the leading edge of the Prometheus flow moved 75 to 95 km (47 to 59 mi) between Voyager in 1979 and the first Galileo observations in 1996. A major eruption in 1997 produced more than 3,500 km2 (1,400 sq mi) of fresh lava and flooded the floor of the adjacent Pillan Patera.[56]

Analysis of the Voyager images led scientists to believe that these flows were composed mostly of various compounds of molten sulfur. However, subsequent Earth-based infrared studies and measurements from the Galileo spacecraft indicate that these flows are composed of basaltic lava with mafic to ultramafic compositions.[124] This hypothesis is based on temperature measurements of Io's "hotspots", or thermal-emission locations, which suggest temperatures of at least 1,300 K and some as high as 1,600 K.[125] Initial estimates suggesting eruption temperatures approaching 2,000 K[56] have since proven to be overestimates because the wrong thermal models were used to model the temperatures.[125][124]

Five-image sequence of New Horizons images showing Io's volcano Tvashtar spewing material 330 km above its surface

The discovery of plumes at the volcanoes Pele and Loki were the first sign that Io is geologically active.[48] Generally, these plumes are formed when volatiles like sulfur and sulfur dioxide are ejected skyward from Io's volcanoes at speeds reaching 1 km/s (0.62 mi/s), creating umbrella-shaped clouds of gas and dust. Additional material that might be found in these volcanic plumes include sodium, potassium, and chlorine.[126][127] These plumes appear to be formed in one of two ways.[128] Io's largest plumes, such as those emitted by Pele, are created when dissolved sulfur and sulfur dioxide gas are released from erupting magma at volcanic vents or lava lakes, often dragging silicate pyroclastic material with them.[129] These plumes form red (from the short-chain sulfur) and black (from the silicate pyroclastics) deposits on the surface. Plumes formed in this manner are among the largest observed at Io, forming red rings more than 1,000 km (620 mi) in diameter. Examples of this plume type include Pele, Tvashtar, and Dazhbog. Another type of plume is produced when encroaching lava flows vaporize underlying sulfur dioxide frost, sending the sulfur skyward. This type of plume often forms bright circular deposits consisting of sulfur dioxide. These plumes are often less than 100 km (62 mi) tall, and are among the most long-lived plumes on Io. Examples include Prometheus, Amirani, and Masubi. The erupted sulfurous compounds are concentrated in the upper crust from a decrease in sulfur solubility at greater depths in Io's lithosphere and can be a determinant for the eruption style of a hot spot.[129][130][131]


Main article: Mountains of Io

See also: List of mountains on Io

Galileo greyscale image of Tohil Mons, a 5.4-km-tall mountain

Io has 100 to 150 mountains. These structures average 6 km (3.7 mi) in height and reach a maximum of 17.5 ± 1.5 km (10.9 ± 0.9 mi) at South Boösaule Montes.[14] Mountains often appear as large (the average mountain is 157 km or 98 mi long), isolated structures with no apparent global tectonic patterns outlined, in contrast to the case on Earth.[14] To support the tremendous topography observed at these mountains requires compositions consisting mostly of silicate rock, as opposed to sulfur.[132]

"Steeple Mountain" on moon Io
(animation; JunoCam; 0:14; 18 April 2024)

Despite the extensive volcanism that gives Io its distinctive appearance, nearly all of its mountains are tectonic structures, and are not produced by volcanoes. Instead, most Ionian mountains form as the result of compressive stresses on the base of the lithosphere, which uplift and often tilt chunks of Io's crust through thrust faulting.[133] The compressive stresses leading to mountain formation are the result of subsidence from the continuous burial of volcanic materials.[133] The global distribution of mountains appears to be opposite that of volcanic structures; mountains dominate areas with fewer volcanoes and vice versa.[134] This suggests large-scale regions in Io's lithosphere where compression (supportive of mountain formation) and extension (supportive of patera formation) dominate.[135] Locally, however, mountains and paterae often abut one another, suggesting that magma often exploits faults formed during mountain formation to reach the surface.[116]

Mountains on Io (generally, structures rising above the surrounding plains) have a variety of morphologies. Plateaus are most common.[14] These structures resemble large, flat-topped mesas with rugged surfaces. Other mountains appear to be tilted crustal blocks, with a shallow slope from the formerly flat surface and a steep slope consisting of formerly sub-surface materials uplifted by compressive stresses. Both types of mountains often have steep scarps along one or more margins. Only a handful of mountains on Io appear to have a volcanic origin. These mountains resemble small shield volcanoes, with steep slopes (6–7°) near a small, central caldera and shallow slopes along their margins.[136] These volcanic mountains are often smaller than the average mountain on Io, averaging only 1 to 2 km (0.6 to 1.2 mi) in height and 40 to 60 km (25 to 37 mi) wide. Other shield volcanoes with much shallower slopes are inferred from the morphology of several of Io's volcanoes, where thin flows radiate out from a central patera, such as at Ra Patera.[136]

Nearly all mountains appear to be in some stage of degradation. Large landslide deposits are common at the base of Ionian mountains, suggesting that mass wasting is the primary form of degradation. Scalloped margins are common among Io's mesas and plateaus, the result of sulfur dioxide sapping from Io's crust, producing zones of weakness along mountain margins.[137]


Main article: Atmosphere of Io

Auroral glows in Io's upper atmosphere. Different colors represent emission from different components of the atmosphere (green comes from emitting sodium, red from emitting oxygen, and blue from emitting volcanic gases like sulfur dioxide). Image taken while Io was in eclipse.

Io has an extremely thin atmosphere consisting mainly of sulfur dioxide (SO
), with minor constituents including sulfur monoxide (SO), sodium chloride (NaCl), and atomic sulfur and oxygen.[138] The atmosphere has significant variations in density and temperature with time of day, latitude, volcanic activity, and surface frost abundance. The maximum atmospheric pressure on Io ranges from 3.3 × 10−5 to 3 × 10−4 pascals (Pa) or 0.3 to 3 nbar, spatially seen on Io's anti-Jupiter hemisphere and along the equator, and temporally in the early afternoon when the temperature of surface frost peaks.[138][139][140] Localized peaks at volcanic plumes have also been seen, with pressures of 5 × 10−4 to 40  × 10−4 Pa (5 to 40 nbar).[52] Io's atmospheric pressure is lowest on Io's night side, where the pressure dips to 0.1 × 10−7 to 1 × 10−7 Pa (0.0001 to 0.001 nbar).[138][139] Io's atmospheric temperature ranges from the temperature of the surface at low altitudes, where sulfur dioxide is in vapor pressure equilibrium with frost on the surface, to 1,800 K at higher altitudes where the lower atmospheric density permits heating from plasma in the Io plasma torus and from Joule heating from the Io flux tube.[138][139] The low pressure limits the atmosphere's effect on the surface, except for temporarily redistributing sulfur dioxide from frost-rich to frost-poor areas, and to expand the size of plume deposit rings when plume material re-enters the thicker dayside atmosphere.[138][139]

Gas in Io's atmosphere is stripped by Jupiter's magnetosphere, escaping to either the neutral cloud that surrounds Io, or the Io plasma torus, a ring of ionized particles that shares Io's orbit but co-rotates with the magnetosphere of Jupiter.[82] Approximately one ton of material is removed from the atmosphere every second through this process so that it must be constantly replenished.[78] The most dramatic source of SO
are volcanic plumes, which pump 104 kg of sulfur dioxide per second into Io's atmosphere on average, though most of this condenses back onto the surface.[141] Much of the sulfur dioxide in Io's atmosphere is sustained by sunlight-driven sublimation of SO
frozen on the surface.[142] The day-side atmosphere is largely confined to within 40° of the equator, where the surface is warmest and most active volcanic plumes reside.[143] A sublimation-driven atmosphere is also consistent with observations that Io's atmosphere is densest over the anti-Jupiter hemisphere, where SO
frost is most abundant, and is densest when Io is closer to the Sun.[138][142][144] However, some contributions from volcanic plumes are required as the highest observed densities have been seen near volcanic vents.[138] Because the density of sulfur dioxide in the atmosphere is tied directly to surface temperature, Io's atmosphere partially collapses at night, or when Io is in the shadow of Jupiter (with an ~80% drop in column density[145]). The collapse during eclipse is limited somewhat by the formation of a diffusion layer of sulfur monoxide in the lowest portion of the atmosphere, but the atmosphere pressure of Io's nightside atmosphere is two to four orders of magnitude less than at its peak just past noon.[139][146] The minor constituents of Io's atmosphere, such as NaCl, SO, O, and S derive either from: direct volcanic outgassing; photodissociation, or chemical breakdown caused by solar ultraviolet radiation, from SO
; or the sputtering of surface deposits by charged particles from Jupiter's magnetosphere.[142]

Various researchers have proposed that the atmosphere of Io freezes onto the surface when it passes into the shadow of Jupiter. Evidence for this is a "post-eclipse brightening", where the moon sometimes appears a bit brighter as if covered with frost immediately after eclipse. After about 15 minutes the brightness returns to normal, presumably because the frost has disappeared through sublimation.[147][148][149][150] Besides being seen through ground-based telescopes, post-eclipse brightening was found in near-infrared wavelengths using an instrument aboard the Cassini spacecraft.[151] Further support for this idea came in 2013 when the Gemini Observatory was used to directly measure the collapse of Io's SO2 atmosphere during, and its reformation after, eclipse with Jupiter.[152][153]

High-resolution images of Io acquired when Io is experiencing an eclipse reveal an aurora-like glow.[127] As on Earth, this is due to particle radiation hitting the atmosphere, though in this case the charged particles come from Jupiter's magnetic field rather than the solar wind. Aurorae usually occur near the magnetic poles of planets, but Io's are brightest near its equator. Io lacks an intrinsic magnetic field of its own; therefore, electrons traveling along Jupiter's magnetic field near Io directly impact Io's atmosphere. More electrons collide with its atmosphere, producing the brightest aurora, where the field lines are tangent to Io (i.e. near the equator), because the column of gas they pass through is the longest there. Aurorae associated with these tangent points on Io are observed to rock with the changing orientation of Jupiter's tilted magnetic dipole.[154] Fainter aurora from oxygen atoms along the limb of Io (the red glows in the image at right), and sodium atoms on Io's night-side (the green glows in the same image) have also been observed.[127]

See also


  1. ^ a b Blue, Jennifer (9 November 2009). "Planet and Satellite Names and Discoverers". USGS.
  2. ^ "Io". Lexico UK English Dictionary. Oxford University Press. Archived from the original on 29 February 2020.
    "Io". Dictionary.
  3. ^ S. W. Kieffer (1982) "Ionian Volcanism", in David Morrison, ed., Satellites of Jupiter, vol. 3, International Astronomical Union
  4. ^ "Electron Beams and Ion Composition Measured at Io and in Its Torus", Science, 1996 October 18
  5. ^ 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.
  6. ^ a b c d Yeomans, Donald K. (13 July 2006). "Planetary Satellite Physical Parameters". JPL Solar System Dynamics.
  7. ^ a b 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.
  8. ^ 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.
  9. ^ "Classic Satellites of the Solar System". Observatorio ARVAL. Archived from the original on 9 July 2011. Retrieved 28 September 2007.
  10. ^ "Io". 5 December 2001. Retrieved 21 May 2022.
  11. ^ a b Rosaly MC Lopes (2006). "Io: The Volcanic Moon". In Lucy-Ann McFadden; Paul R. Weissman; Torrence V. Johnson (eds.). Encyclopedia of the Solar System. Academic Press. pp. 419–431. ISBN 978-0-12-088589-3.
  12. ^ a b 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.
  13. ^ a b Sokol, Joshua (26 June 2019). "This World Is a Simmering Hellscape. They've Been Watching Its Explosions. - Researchers have released a five-year record of volcanic activity on Io, a moon of Jupiter, hoping others will find more patterns". The New York Times. Retrieved 26 June 2019.
  14. ^ a b c d Schenk, P.; et al. (2001). "The Mountains of Io: Global and Geological Perspectives from Voyager and Galileo". Journal of Geophysical Research. 106 (E12): 33201–33222. Bibcode:2001JGR...10633201S. doi:10.1029/2000JE001408.
  15. ^ "2000 February 29, SPS 1020 (Introduction to Space Sciences)". 29 February 2000. Archived from the original on 25 July 2008.
  16. ^ a b c d Van Helden, Albert (August 1994). "Naming the Satellites of Jupiter and Saturn" (PDF). The Newsletter of the Historical Astronomy Division of the American Astronomical Society (32). Retrieved 10 March 2023.
  17. ^ Marius, S. (1614). "Mundus Iovialis anno M.DC.IX Detectus Ope Perspicilli Belgici" [The World of Jupiter discovered in the year 1609 by Means of a Belgian spy-glass]. The Observatory. 39: 367. Bibcode:1916Obs....39..367.
  18. ^ Van Helden, Al (1995). "Satellites of Jupiter".
  19. ^ Marazzini, Claudio (2005). "I nomi dei satelliti di Giove: da Galileo a Simon Marius" [The names of the satellites of Jupiter: from Galileo to Simon Marius]. Lettere Italiane (in Italian). 57 (3): 391–407. JSTOR 26267017.
  20. ^ "Io: Overview". NASA. Archived from the original on 11 February 2003. Retrieved 5 March 2012.
  21. ^ a b c Barnard, E. E. (1894). "On the Dark Poles and Bright Equatorial Belt of the First Satellite of Jupiter". Monthly Notices of the Royal Astronomical Society. 54 (3): 134–136. Bibcode:1894MNRAS..54..134B. doi:10.1093/mnras/54.3.134.
  22. ^ a b Barnard, E. E. (1891). "Observations of the Planet Jupiter and his Satellites during 1890 with the 12-inch Equatorial of the Lick Observatory". Monthly Notices of the Royal Astronomical Society. 51 (9): 543–556. Bibcode:1891MNRAS..51..543B. doi:10.1093/mnras/51.9.543.
  23. ^ "Io2". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
    "Io". Lexico UK English Dictionary UK English Dictionary. Oxford University Press. Archived from the original on 29 February 2020.
    "Io". Dictionary.
    "Io". Unabridged (Online). n.d.
  24. ^ "Io". Unabridged (Online). n.d.
  25. ^ genitives Iūs and Iōnis: Io2. Charlton T. Lewis and Charles Short. A Latin Dictionary on Perseus Project.
  26. ^ Morrison & Matthews (1982) Satellites of Jupiter, part 1, p. 649
  27. ^ McEwen et al., 'Lithosphere and Surface of Io', Schubert et al., 'Satellite Interiors', and Schenk et al., 'Ages and Interiors', in Bagenal et al. eds. (2007) Jupiter: The Planet, Satellites and Magnetosphere
  28. ^ Outside astronomy, "Ionian" would likely be misunderstood as referring to Ionia, but an adjective based on the other stem, "Ioan" /ˈən/, is not found.
  29. ^ a b Blue, Jennifer. "Categories for Naming Features on Planets and Satellites". U.S. Geological Survey. Retrieved 12 September 2013.
  30. ^ Blue, Jennifer (14 June 2007). "Io Nomenclature Table of Contents". U.S. Geological Survey. Archived from the original on 29 June 2007.
  31. ^ a b c Cruikshank, D. P.; Nelson, R. M. (2007). "A history of the exploration of Io". In Lopes, R. M. C.; Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 5–33. ISBN 978-3-540-34681-4.
  32. ^ Van Helden, Albert (14 January 2004). "The Galileo Project / Science / Simon Marius". Rice University.
  33. ^ Baalke, Ron. "Discovery of the Galilean Satellites". Jet Propulsion Laboratory. Archived from the original on 6 January 1997. Retrieved 7 January 2010.
  34. ^ O'Connor, J. J.; Robertson, E. F. (February 1997). "Longitude and the Académie Royale". University of St. Andrews. Archived from the original on 2 September 2011. Retrieved 14 June 2007.
  35. ^ Keane, J. T.; Matsuyama, Isamu; Bierson, C. J.; Trinh, A. (2023). "Tidal Heating and the Interior Structure of Io". In Lopes, R. M. C.; de Kleer, K.; Keane, J. T. (eds.). Io: A New View of Jupiter's Moon. Springer. pp. 95–146. ISBN 978-3-031-25669-1.
  36. ^ Dobbins, T.; Sheehan, W. (2004). "The Story of Jupiter's Egg Moons". Sky & Telescope. 107 (1): 114–120. Bibcode:2004S&T...107a.114D.
  37. ^ Minton, R. B. (1973). "The Red Polar Caps of Io". Communications of the Lunar and Planetary Laboratory. 10: 35–39. Bibcode:1973CoLPL..10...35M.
  38. ^ Lee, T. (1972). "Spectral Albedos of the Galilean Satellites". Communications of the Lunar and Planetary Laboratory. 9 (3): 179–180. Bibcode:1972CoLPL...9..179L.
  39. ^ Fanale, F. P.; et al. (1974). "Io: A Surface Evaporite Deposit?". Science. 186 (4167): 922–925. Bibcode:1974Sci...186..922F. doi:10.1126/science.186.4167.922. PMID 17730914. S2CID 205532.
  40. ^ a b Bigg, E. K. (1964). "Influence of the Satellite Io on Jupiter's Decametric Emission". Nature. 203 (4949): 1008–1010. Bibcode:1964Natur.203.1008B. doi:10.1038/2031008a0. S2CID 12233914.
  41. ^ a b Fimmel, R. O.; et al. (1977). "First into the Outer Solar System". Pioneer Odyssey. NASA. Retrieved 5 June 2007.
  42. ^ Anderson, J. D.; et al. (1974). "Gravitational parameters of the Jupiter system from the Doppler tracking of Pioneer 10". Science. 183 (4122): 322–323. Bibcode:1974Sci...183..322A. doi:10.1126/science.183.4122.322. PMID 17821098. S2CID 36510719.
  43. ^ "Pioneer 11 Images of Io". Galileo Home Page. Archived from the original on 9 April 1997. Retrieved 21 April 2007.
  44. ^ "Voyager Mission Description". NASA PDS Rings Node. 19 February 1997.
  45. ^ a b c Smith, B. A.; et al. (1979). "The Jupiter system through the eyes of Voyager 1". Science. 204 (4396): 951–972. Bibcode:1979Sci...204..951S. doi:10.1126/science.204.4396.951. PMID 17800430. S2CID 33147728.
  46. ^ "Jupiter moon shows color, erosion signs". The Milwaukee Sentinel. United Press International. 6 March 1979. p. 2.[permanent dead link]
  47. ^ Carr, M. H.; et al. (1980). "Volcanic Features on Io". Nature. 280: 729–733. doi:10.1038/280729a0.
  48. ^ a b Morabito, L. A.; et al. (1979). "Discovery of currently active extraterrestrial volcanism". Science. 204 (4396): 972. Bibcode:1979Sci...204..972M. doi:10.1126/science.204.4396.972. PMID 17800432. S2CID 45693338.
  49. ^ a b Strom, R. G.; et al. (1979). "Volcanic eruption plumes on Io". Nature. 280 (5725): 733–736. Bibcode:1979Natur.280..733S. doi:10.1038/280733a0. S2CID 8798702.
  50. ^ a b c d Peale, S. J.; et al. (1979). "Melting of Io by Tidal Dissipation" (PDF). Science. 203 (4383): 892–894. Bibcode:1979Sci...203..892P. doi:10.1126/science.203.4383.892. PMID 17771724. S2CID 21271617. Archived from the original (PDF) on 11 February 2020.
  51. ^ Soderblom, L. A.; et al. (1980). "Spectrophotometry of Io: Preliminary Voyager 1 results". Geophys. Res. Lett. 7 (11): 963–966. Bibcode:1980GeoRL...7..963S. doi:10.1029/GL007i011p00963.
  52. ^ a b Pearl, J. C.; et al. (1979). "Identification of gaseous SO
    and new upper limits for other gases on Io"
    . Nature. 288 (5725): 757–758. Bibcode:1979Natur.280..755P. doi:10.1038/280755a0. S2CID 4338190.
  53. ^ Broadfoot, A. L.; et al. (1979). "Extreme ultraviolet observations from Voyager 1 encounter with Jupiter". Science. 204 (4396): 979–982. Bibcode:1979Sci...204..979B. doi:10.1126/science.204.4396.979. PMID 17800434. S2CID 1442415.
  54. ^ Strom, R. G.; Schneider, N. M. (1982). "Volcanic eruptions on Io". In Morrison, D. (ed.). Satellites of Jupiter. University of Arizona Press. pp. 598–633. ISBN 0-8165-0762-7.
  55. ^ a b Anderson, J. D.; et al. (1996). "Galileo Gravity Results and the Internal Structure of Io". Science. 272 (5262): 709–712. Bibcode:1996Sci...272..709A. doi:10.1126/science.272.5262.709. PMID 8662566. S2CID 24373080.
  56. ^ a b c McEwen, A. S.; et al. (1998). "High-temperature silicate volcanism on Jupiter's moon Io" (PDF). Science. 281 (5373): 87–90. Bibcode:1998Sci...281...87M. doi:10.1126/science.281.5373.87. PMID 9651251. S2CID 28222050. Archived from the original (PDF) on 23 September 2020.
  57. ^ a b Perry, J.; et al. (2007). "A Summary of the Galileo mission and its observations of Io". In Lopes, R. M. C.; Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 35–59. ISBN 978-3-540-34681-4.
  58. ^ Porco, C. C.; et al. (2003). "Cassini imaging of Jupiter's atmosphere, satellites, and rings" (PDF). Science. 299 (5612): 1541–1547. Bibcode:2003Sci...299.1541P. doi:10.1126/science.1079462. PMID 12624258. S2CID 20150275.
  59. ^ a b Spencer, J. R.; et al. (2007). "Io Volcanism Seen by New Horizons: A Major Eruption of the Tvashtar Volcano" (PDF). Science. 318 (5848): 240–243. Bibcode:2007Sci...318..240S. doi:10.1126/science.1147621. PMID 17932290. S2CID 36446567. Archived from the original (PDF) on 12 April 2020.
  60. ^ "Juno – Mission Overview". NASA. Retrieved 11 March 2024.
  61. ^ a b Mura, A.; et al. (2020). "Infrared observations of Io from Juno". Icarus. 341: 113607. Bibcode:2020Icar..34113607M. doi:10.1016/j.icarus.2019.113607. S2CID 213970081.
  62. ^ "NASA's Juno Mission Expands into the Future". 13 January 2021. Retrieved 1 February 2021.
  63. ^ Miller, Katrina (4 January 2024). "New Images of Jupiter's Moon Io Capture Infernal Volcanic Landscape - Juno, a NASA mission designed to study Jupiter's origins, sent back new views of the most eruptive world in the solar system". The New York Times. Archived from the original on 4 January 2024. Retrieved 4 January 2024.
  64. ^ "Juno to Get Second Close Look at Jupiter's Volcanic Moon Io on Feb. 3". 3 February 2024. Retrieved 11 March 2024.
  65. ^ Bolton, Scott (2 September 2020). "Juno OPAG Report" (PDF). Retrieved 31 August 2020.
  66. ^ Anderson, Paul Scott (6 January 2019). "New Juno images of Io's fiery volcanoes". EarthSky. Retrieved 14 February 2020.
  67. ^ Tosi, F.; et al. (2020). "Mapping Io's Surface Composition With Juno/JIRAM". Journal of Geophysical Research: Planets. 125 (11): e06522. Bibcode:2020JGRE..12506522T. doi:10.1029/2020JE006522. S2CID 225456943.
  68. ^ Jonathan Amos (2 May 2012). "Esa selects 1bn-euro Juice probe to Jupiter". BBC News.
  69. ^ Witasse, O.; Altobelli, N.; Andres, R.; Atzei, A.; Boutonnet, A.; Budnik, F.; Dietz, A.; Erd, C.; Evill, R.; Lorente, R.; Munoz, C.; Pinzan, G.; Scharmberg, C.; Suarez, A.; Tanco, I.; Torelli, F.; Torn, B.; Vallat, C.; JUICE Science Working Team (July 2021). JUICE (Jupiter Icy Moon Explorer): Plans for the cruise phase. Europlanet Science Congress (EPSC) 2021. doi:10.5194/epsc2021-358. Retrieved 28 August 2021.
  70. ^ JUICE assessment study report (Yellow Book), ESA, 2012
  71. ^ "Europa Clipper Mission Overview". Jet Propulsion Laboratory. Retrieved 22 December 2022.
  72. ^ McEwen, A. S.; IVO Team (2021). The Io Volcano Observer (IVO) (PDF). 52nd Lunar and Planetary Science Conference. 15–19 March 2020. Abstract #2548.
  73. ^ "NASA Selects Four Possible Missions to Study the Secrets of the Solar System". NASA. 13 February 2020.
  74. ^ Strickland, Ashley (3 June 2021). "Two new NASA missions will uncover the secrets of Venus". CNN.
  75. ^ Lopes, R. M. C.; Williams, D. A. (2005). "Io after Galileo". Reports on Progress in Physics. 68 (2): 303–340. Bibcode:2005RPPh...68..303L. doi:10.1088/0034-4885/68/2/R02. S2CID 44208045.
  76. ^ Spencer, J. "John Spencer's Astronomical Visualizations". Retrieved 25 May 2007.
  77. ^ "Io: Overview". Solar System Exploration. NASA. Archived from the original on 11 February 2003. Retrieved 29 October 2014.
  78. ^ a b c d e f g h Schneider, N. M.; Bagenal, F. (2007). "Io's neutral clouds, plasma torus, and magnetospheric interactions". In Lopes, R. M. C.; Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 265–286. ISBN 978-3-540-34681-4.
  79. ^ a b Postberg, F.; et al. (2006). "Composition of jovian dust stream particles". Icarus. 183 (1): 122–134. Bibcode:2006Icar..183..122P. doi:10.1016/j.icarus.2006.02.001.
  80. ^ a b Bagenal, F.; Dols, V. (2023). "Space Environment of Io". In Lopes, R. M. C.; de Kleer, K.; Keane, J. T. (eds.). Io: A New View of Jupiter's Moon. Springer. pp. 291–322. ISBN 978-3-031-25669-1.
  81. ^ Burger, M. H.; et al. (1999). "Galileo's close-up view of Io sodium jet". Geophys. Res. Lett. 26 (22): 3333–3336. Bibcode:1999GeoRL..26.3333B. doi:10.1029/1999GL003654.
  82. ^ a b Krimigis, S. M.; et al. (2002). "A nebula of gases from Io surrounding Jupiter". Nature. 415 (6875): 994–996. Bibcode:2002Natur.415..994K. doi:10.1038/415994a. PMID 11875559.
  83. ^ Medillo, M.; et al. (2004). "Io's volcanic control of Jupiter's extended neutral clouds". Icarus. 170 (2): 430–442. Bibcode:2004Icar..170..430M. doi:10.1016/j.icarus.2004.03.009.
  84. ^ Grün, E.; et al. (1993). "Discovery of Jovian dust streams and interstellar grains by the ULYSSES spacecraft". Nature. 362 (6419): 428–430. Bibcode:1993Natur.362..428G. doi:10.1038/362428a0. S2CID 4315361.
  85. ^ Zook, H. A.; et al. (1996). "Solar Wind Magnetic Field Bending of Jovian Dust Trajectories". Science. 274 (5292): 1501–1503. Bibcode:1996Sci...274.1501Z. doi:10.1126/science.274.5292.1501. PMID 8929405. S2CID 25816078.
  86. ^ Grün, E.; et al. (1996). "Dust Measurements During Galileo's Approach to Jupiter and Io Encounter". Science. 274 (5286): 399–401. Bibcode:1996Sci...274..399G. doi:10.1126/science.274.5286.399. S2CID 119868296.
  87. ^ a b Khurana, Krishan K.; Jia, Xianzhe; Kivelson, Margaret G.; Nimmo, Francis; Schubert, Gerald; Russell, Christopher T. (3 June 2011). "Evidence of a Global Magma Ocean in Io's Interior". Science. 332 (6034): 1186–1189. Bibcode:2011Sci...332.1186K. doi:10.1126/science.1201425. PMID 21566160. S2CID 19389957.
  88. ^ Khurana, K. K.; et al. (1998). "Induced magnetic fields as evidence for subsurface oceans in Europa and Callisto". Nature. 395: 777–780. doi:10.1038/27394.
  89. ^ Schneider, N. M.; Spencer, J. R. (2023). "Understanding Io: Four Centuries of Study and Surprise". In Lopes, R. M. C.; de Kleer, K.; Keane, J. T. (eds.). Io: A New View of Jupiter's Moon. Springer. pp. 9–40. ISBN 978-3-031-25669-1.
  90. ^ a b Anderson, J. D.; et al. (2001). "Io's gravity field and interior structure". J. Geophys. Res. 106 (E12): 32963–32969. Bibcode:2001JGR...10632963A. doi:10.1029/2000JE001367.
  91. ^ Kivelson, M. G.; et al. (2001). "Magnetized or Unmagnetized: Ambiguity persists following Galileo's encounters with Io in 1999 and 2000". J. Geophys. Res. 106 (A11): 26121–26135. Bibcode:2001JGR...10626121K. doi:10.1029/2000JA002510.
  92. ^ Sohl, F.; et al. (2002). "Implications from Galileo observations on the interior structure and chemistry of the Galilean satellites". Icarus. 157 (1): 104–119. Bibcode:2002Icar..157..104S. doi:10.1006/icar.2002.6828.
  93. ^ Kuskov, O. L.; Kronrod, V. A. (2001). "Core sizes and internal structure of the Earth's and Jupiter's satellites". Icarus. 151 (2): 204–227. Bibcode:2001Icar..151..204K. doi:10.1006/icar.2001.6611.
  94. ^ a b c d Moore, W. B.; et al. (2007). "The Interior of Io.". In R. M. C. Lopes; J. R. Spencer (eds.). Io after Galileo. Springer-Praxis. pp. 89–108. ISBN 978-3-540-34681-4.
  95. ^ "NASA's Galileo Reveals Magma 'Ocean' Beneath Surface of Jupiter's Moon". Science Daily. 12 May 2011.
  96. ^ Perry, J. (21 January 2010). "Science: Io's Induced Magnetic Field and Mushy Magma Ocean". The Gish Bar Times.
  97. ^ Jaeger, W. L.; et al. (2003). "Orogenic tectonism on Io". J. Geophys. Res. 108 (E8): 12–1. Bibcode:2003JGRE..108.5093J. doi:10.1029/2002JE001946.
  98. ^ Yoder, C. F.; et al. (1979). "How tidal heating in Io drives the Galilean orbital resonance locks". Nature. 279 (5716): 767–770. Bibcode:1979Natur.279..767Y. doi:10.1038/279767a0. S2CID 4322070.
  99. ^ "Interplanetary Low Tide - NASA Science Mission Directorate". Archived from the original on 4 June 2023. Retrieved 16 October 2019.
  100. ^ a b Lainey, V.; et al. (2009). "Strong tidal dissipation in Io and Jupiter from astrometric observations". Nature. 459 (7249): 957–959. Bibcode:2009Natur.459..957L. doi:10.1038/nature08108. PMID 19536258. S2CID 205217186.
  101. ^ Moore, W. B. (August 2003). "Tidal heating and convection in Io". Journal of Geophysical Research. 108 (E8): 5096. Bibcode:2003JGRE..108.5096M. doi:10.1029/2002JE001943. S2CID 53443229.
  102. ^ Steigerwald, William (10 September 2015). "Underground Magma Ocean Could Explain Io's 'Misplaced' Volcanoes". NASA. Retrieved 19 September 2015.
  103. ^ Tyler, Robert H.; Henning, Wade G.; Hamilton, Christopher W. (June 2015). "Tidal Heating in a Magma Ocean within Jupiter's Moon Io". The Astrophysical Journal Supplement Series. 218 (2). 22. Bibcode:2015ApJS..218...22T. doi:10.1088/0067-0049/218/2/22. hdl:11603/28862.
  104. ^ Lewin, Sarah (14 September 2015). "Magma Oceans on Jupiter's Moon Io May Solve Volcano Mystery". Retrieved 19 September 2015.
  105. ^ "Cassini Finds Global Ocean in Saturn's Moon Enceladus". NASA / Jet Propulsion Laboratory. 15 September 2015. Retrieved 19 September 2015.
  106. ^ Britt, Robert Roy (16 March 2000). "Pizza Pie in the Sky: Understanding Io's Riot of Color". Archived from the original on 18 August 2000.
  107. ^ Calder, Nigel (2005). Magic Universe: A Grand Tour of Modern Science. Oxford University Press. p. 215. ISBN 978-0-19-280669-7.
  108. ^ a b Carlson, R. W.; et al. (2007). "Io's surface composition". In Lopes, R. M. C.; Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 194–229. ISBN 978-3-540-34681-4.
  109. ^ Spencer, J.; et al. (2000). "Discovery of Gaseous S2 in Io's Pele Plume". Science. 288 (5469): 1208–1210. Bibcode:2000Sci...288.1208S. doi:10.1126/science.288.5469.1208. PMID 10817990.
  110. ^ Kieffer, S. W.; et al. (2000). "Prometheus: Io's Wandering Plume". Science. 288 (5469): 1204–1208. doi:10.1126/science.288.5469.1204.
  111. ^ Douté, S.; et al. (2004). "Geology and activity around volcanoes on Io from the analysis of NIMS". Icarus. 169 (1): 175–196. Bibcode:2004Icar..169..175D. doi:10.1016/j.icarus.2004.02.001.
  112. ^ Seeds, Michael A.; Backman, Dana E. (2012). The Solar System (8th ed.). Cengage Learning. p. 514. ISBN 9781133713685.
  113. ^ Hadhazy, Adam (6 March 2014). "Alien Moons Could Bake Dry from Young Gas Giants' Hot Glow". Astrobiology Magazine. Archived from the original on 31 August 2015. Retrieved 28 October 2014.((cite news)): CS1 maint: unfit URL (link)
  114. ^ Keszthelyi, L. P.; Suer, T. (2023). "The Composition of Io". In Lopes, R. M. C.; de Kleer, K.; Keane, J. T. (eds.). Io: A New View of Jupiter's Moon. Springer. pp. 211–232. ISBN 978-3-031-25669-1.
  115. ^ "Looking Into Io's Loki Patera (Artist's Concept)". NASA/JPL. 18 April 2024. Retrieved 25 April 2024.
  116. ^ a b c d Radebaugh, D.; et al. (2001). "Paterae on Io: A new type of volcanic caldera?" (PDF). J. Geophys. Res. 106 (E12): 33005–33020. Bibcode:2001JGR...10633005R. doi:10.1029/2000JE001406.
  117. ^ Keszthelyi, L.; et al. (2004). "A Post-Galileo view of Io's Interior". Icarus. 169 (1): 271–286. Bibcode:2004Icar..169..271K. doi:10.1016/j.icarus.2004.01.005.
  118. ^ Williams, David; Radebaugh, Jani; Keszthelyi, Laszlo P.; McEwen, Alfred S.; Lopes, Rosaly M. C.; Douté, Sylvain; Greeley, Ronald (2002). "Geologic mapping of the Chaac-Camaxtli region of Io from Galileo imaging data". Journal of Geophysical Research. 107 (E9): 5068. Bibcode:2002JGRE..107.5068W. doi:10.1029/2001JE001821. S2CID 41607277.
  119. ^ Moore, Patrick, ed. (2002). Astronomy Encyclopedia. New York: Oxford University Press. p. 232. ISBN 0-19-521833-7.
  120. ^ Perry, J. E.; et al. (2003). Gish Bar Patera, Io: Geology and Volcanic Activity, 1997–2001 (PDF). LPSC XXXIV. Clear Lake City (Greater Houston). Abstract #1720.
  121. ^ Radebaugh, J.; et al. (2004). "Observations and temperatures of Io's Pele Patera from Cassini and Galileo spacecraft images". Icarus. 169 (1): 65–79. Bibcode:2004Icar..169...65R. doi:10.1016/j.icarus.2003.10.019.
  122. ^ Howell, R. R.; Lopes, R. M. C. (2007). "The nature of the volcanic activity at Loki: Insights from Galileo NIMS and PPR data". Icarus. 186 (2): 448–461. Bibcode:2007Icar..186..448H. doi:10.1016/j.icarus.2006.09.022.
  123. ^ Keszthelyi, L.; et al. (2001). "Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission". J. Geophys. Res. 106 (E12): 33025–33052. Bibcode:2001JGR...10633025K. doi:10.1029/2000JE001383.
  124. ^ a b Battaglia, Steven M. (March 2019). A Jökulhlaup-like Model for Secondary Sulfur Flows on Io. 50th Lunar and Planetary Science Conference. 18–22 March 2019. The Woodlands, Texas. Bibcode:2019LPI....50.1189B. LPI Contribution No. 1189.
  125. ^ a b Keszthelyi, L.; et al. (2007). "New estimates for Io eruption temperatures: Implications for the interior". Icarus. 192 (2): 491–502. Bibcode:2007Icar..192..491K. doi:10.1016/j.icarus.2007.07.008.
  126. ^ Roesler, F. L.; Moos, H. W.; Oliversen, R. J.; Woodward, Jr., R. C.; Retherford, K. D.; et al. (January 1999). "Far-Ultraviolet Imaging Spectroscopy of Io's Atmosphere with HST/STIS". Science. 283 (5400): 353–357. Bibcode:1999Sci...283..353R. doi:10.1126/science.283.5400.353. PMID 9888844.
  127. ^ a b c Geissler, P. E.; McEwen, A. S.; Ip, W.; Belton, M. J. S.; Johnson, T. V.; et al. (August 1999). "Galileo Imaging of Atmospheric Emissions from Io" (PDF). Science. 285 (5429): 870–874. Bibcode:1999Sci...285..870G. doi:10.1126/science.285.5429.870. PMID 10436151. S2CID 33402233. Archived from the original (PDF) on 20 February 2019.
  128. ^ McEwen, A. S.; Soderblom, L. A. (August 1983). "Two classes of volcanic plume on Io". Icarus. 55 (2): 197–226. Bibcode:1983Icar...55..191M. doi:10.1016/0019-1035(83)90075-1.
  129. ^ a b Battaglia, Steven M.; Stewart, Michael A.; Kieffer, Susan W. (June 2014). "Io's theothermal (sulfur) - Lithosphere cycle inferred from sulfur solubility modeling of Pele's magma supply". Icarus. 235: 123–129. Bibcode:2014Icar..235..123B. doi:10.1016/j.icarus.2014.03.019.
  130. ^ Battaglia, Steven M. (March 2015). Io: The role of Sulfide Droplet Nucleation in Pele-Type Volcanism. 46th Lunar and Planetary Science Conference. 16–20 March 2015. The Woodlands, Texas. Bibcode:2015LPI....46.1044B. LPI Contribution No. 1832.
  131. ^ Battaglia, Steven M. (March 2018). Does Io have a Lopsided Asthenosphere? Insights from Katla's Magma Plumbing System, Iceland. 49th Lunar and Planetary Science Conference. 19–23 March 2018. The Woodlands, Texas. Bibcode:2018LPI....49.1047B. LPI Contribution No. 1047.
  132. ^ Clow, G. D.; Carr, M. H. (1980). "Stability of sulfur slopes on Io". Icarus. 44 (2): 268–279. Bibcode:1980Icar...44..268C. doi:10.1016/0019-1035(80)90022-6.
  133. ^ a b Schenk, P. M.; Bulmer, M. H. (1998). "Origin of mountains on Io by thrust faulting and large-scale mass movements" (PDF). Science. 279 (5356): 1514–1517. Bibcode:1998Sci...279.1514S. doi:10.1126/science.279.5356.1514. PMID 9488645. S2CID 8518290. Archived from the original (PDF) on 19 February 2019.
  134. ^ McKinnon, W. B.; et al. (2001). "Chaos on Io: A model for formation of mountain blocks by crustal heating, melting, and tilting" (PDF). Geology. 29 (2): 103–106. Bibcode:2001Geo....29..103M. doi:10.1130/0091-7613(2001)029<0103:COIAMF>2.0.CO;2. S2CID 140149197. Archived from the original (PDF) on 11 February 2020.
  135. ^ Tackley, P. J. (2001). "Convection in Io's asthenosphere: Redistribution of nonuniform tidal heating by mean flows". J. Geophys. Res. 106 (E12): 32971–32981. Bibcode:2001JGR...10632971T. doi:10.1029/2000JE001411. S2CID 130527846.
  136. ^ a b Schenk, P. M.; Wilson, R. R.; Davies, A. G. (2004). "Shield volcano topography and the rheology of lava flows on Io". Icarus. 169 (1): 98–110. Bibcode:2004Icar..169...98S. doi:10.1016/j.icarus.2004.01.015.
  137. ^ Moore, J. M.; et al. (2001). "Landform degradation and slope processes on Io: The Galileo view" (PDF). J. Geophys. Res. 106 (E12): 33223–33240. Bibcode:2001JGR...10633223M. doi:10.1029/2000JE001375. Archived from the original (PDF) on 18 July 2019. Retrieved 25 August 2019.
  138. ^ a b c d e f g Lellouch, E.; et al. (2007). "Io's atmosphere". In Lopes, R. M. C.; and Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 231–264. ISBN 978-3-540-34681-4.
  139. ^ a b c d e Walker, A. C.; et al. (2010). "A Comprehensive Numerical Simulation of Io's Sublimation-Driven Atmosphere". Icarus. in. press (1): 409–432. Bibcode:2010Icar..207..409W. doi:10.1016/j.icarus.2010.01.012.
  140. ^ Spencer, A. C.; et al. (2005). "Mid-infrared detection of large longitudinal asymmetries in Io's SO
    (PDF). Icarus. 176 (2): 283–304. Bibcode:2005Icar..176..283S. doi:10.1016/j.icarus.2005.01.019.
  141. ^ Geissler, P. E.; Goldstein, D. B. (2007). "Plumes and their deposits". In Lopes, R. M. C.; Spencer, J. R. (eds.). Io after Galileo. Springer-Praxis. pp. 163–192. ISBN 978-3-540-34681-4.
  142. ^ a b c Moullet, A.; et al. (2010). "Simultaneous mapping of SO2, SO, NaCl in Io's atmosphere with the Submillimeter Array". Icarus. press (1): 353–365. Bibcode:2010Icar..208..353M. doi:10.1016/j.icarus.2010.02.009.
  143. ^ Feaga, L. M.; et al. (2009). "Io's dayside SO
    atmosphere". Icarus. 201 (2): 570–584. Bibcode:2009Icar..201..570F. doi:10.1016/j.icarus.2009.01.029.
  144. ^ Spencer, John (8 June 2009). "Aloha, Io". The Planetary Society Blog. The Planetary Society.
  145. ^ Tsang, C. C. C.; Spencer, J. R.; Lellouch, E.; Lopez-Valverde, M. A.; Richter, M. J. (2 August 2016). "The collapse of Io's primary atmosphere in Jupiter eclipse". Journal of Geophysical Research: Planets. 121 (8): 1400–1410. Bibcode:2016JGRE..121.1400T. doi:10.1002/2016JE005025. hdl:10261/143708. S2CID 19544014.
  146. ^ Moore, C. H.; et al. (2009). "1-D DSMC simulation of Io's atmospheric collapse and reformation during and after eclipse". Icarus. 201 (2): 585–597. Bibcode:2009Icar..201..585M. doi:10.1016/j.icarus.2009.01.006.
  147. ^ Fanale, F. P.; et al. (June 1981). "Io: Could SO2 condensation/sublimation cause the sometimes reported post-eclipse brightening?". Geophysical Research Letters. 8 (6): 625–628. Bibcode:1981GeoRL...8..625F. doi:10.1029/GL008i006p00625.
  148. ^ Nelson, Robert M.; et al. (February 1993). "The Brightness of Jupiter's Satellite Io Following Emergence from Eclipse: Selected Observations, 1981–1989". Icarus. 101 (2): 223–233. Bibcode:1993Icar..101..223N. doi:10.1006/icar.1993.1020.
  149. ^ Veverka, J.; et al. (July 1981). "Voyager search for posteclipse brightening on Io". Icarus. 47 (1): 60–74. Bibcode:1981Icar...47...60V. doi:10.1016/0019-1035(81)90091-9.
  150. ^ Secosky, James J.; Potter, Michael (September 1994). "A Hubble Space Telescope study of posteclipse brightening and albedo changes on Io". Icarus. 111 (1): 73–78. Bibcode:1994Icar..111...73S. doi:10.1006/icar.1994.1134.
  151. ^ Bellucci, Giancarlo; et al. (November 2004). "Cassini/VIMS observation of an Io post-eclipse brightening event". Icarus. 172 (1): 141–148. Bibcode:2004Icar..172..141B. doi:10.1016/j.icarus.2004.05.012.
  152. ^ Crowe, Robert (2 August 2016). "SwRI Space Scientists Observe Io's Atmospheric Collapse During Eclipse". Southwest Research Institute. Retrieved 4 October 2018.
  153. ^ Tsang, Constantine C. C.; et al. (August 2016). "The collapse of Io's primary atmosphere in Jupiter eclipse" (PDF). Journal of Geophysical Research: Planets. 121 (8): 1400–1410. Bibcode:2016JGRE..121.1400T. doi:10.1002/2016JE005025. hdl:10261/143708. S2CID 19544014.
  154. ^ Retherford, K. D.; et al. (2000). "Io's Equatorial Spots: Morphology of Neutral UV Emissions". J. Geophys. Res. 105 (A12): 27, 157–27, 165. Bibcode:2000JGR...10527157R. doi:10.1029/2000JA002500.

[[Ca tegory:Articles containing video clips]]