2nd Largest Moon of Neptune - Proteus (6th Moon outwards from Neptune)

Discovery

Proteus is the second largest Neptunian moon, and Neptune's largest inner satellite. Proteus is the 19th largest moon of the solar system.

Proteus was discovered from the images taken by Voyager 2 space probe two months before its Neptune flyby in August 1989. It received the temporary designation S/1989 N 1.

Naming

On 16 September 1991 S/1989 N 1 was named after Proteus, the shape-changing sea god of Greek mythology.

Stats

Diameter (mean): 420 km

Semi-major axis: 117,646 km

Orbital Period: 1.12 days

Orbit

Proteus orbits Neptune at the distance approximately equal to 4.75 equatorial radii of the planet. Its orbit has a small eccentricity and is inclined by about 0.5° to the planet's equator.

Proteus is the largest of the regular prograde satellites of Neptune. It rotates synchronously with the orbital motion, which means that one face always points to the planet.

Origin

Proteus, like the other inner satellites of Neptune, is unlikely to be an original body that formed with it, more probably having accreted from the wreak rubble that remained after Triton's capture.

Triton's orbit upon capture would have been highly eccentric, and would have caused chaotic perturbations in the orbits of the original inner Neptunian satellites, causing them to collide and reduce to a disc of rubble. Only after Triton's orbit became circularised did some of the rubble disc re-accrete into the present-day satellites.

Physical characteristics

Proteus, although about 420 km in diameter, is not spherical in shape. The shape of Proteus is close to a sphere with the radius of about 210 km, although deviations from the spherical shape are large—up to 20 km.

Scientists believe it is about as large as a body of its density can be without being pulled into a perfect spherical shape by its own gravity.

Proteus is slightly elongated in the direction of Neptune, although its overall the shape is closer to an irregular polyhedron than to a triaxial ellipsoid.

2nd Largest Moon of Uranus - Oberon (18th Moon outwards from Uranus)

Oberon is the second largest of the Uranus moons and the tenth largest moon in the Solar System.

Discovery

Oberon was spotted by Sir William Herschel on January 11, 1787, six years after he had discovered the planet itself, on the same day he discovered Uranus's largest moon, Titania.

Naming

Oberon is named after the mythical king of the fairies who appears as a character in Shakespeare's A Midsummer Night's Dream.

Stats

Diameter: 1,522 km

Semi-major axis: 583,520 km

Orbital Period: 13.46 days

Orbit

Oberon orbits Uranus at a distance of about 583,520 km, being the farthest from the planet among its five major moons. Its orbital period is around 13.5 days, coincident with its rotational period. In other words, Oberon is a synchronous satellite, tidally locked, with one face always pointing toward the planet.

Oberon spends a significant part of its orbit outside the Uranian magnetosphere. As a result, its surface is directly struck by the solar wind.

Formation

Oberon probably formed from an accretion disk that surrounded the planet just after its formation.

The initial accretional heating together with continued decay of radioactive elements were probably strong enough to melt the ice if some antifreeze like ammonia (in the form of ammonia hydrate) or some salt was present.

Further melting may have led to the separation of ice from rocks and formation of a rocky core surrounded by an icy mantle. A layer of liquid water ('ocean') rich in dissolved ammonia may have formed at the core–mantle boundary.

The eutectic temperature of this mixture is 176 K. If the temperature dropped below this value the ocean would have frozen by now. Freezing of the water would have led to expansion of the interior, which may have also contributed to the formation of canyon-like graben. Still, present knowledge of the evolution of Oberon is very limited.

Exploration Status

So far the only close-up images of Oberon have been from the Voyager 2 probe, which photographed the moon during its flyby of Uranus in January 1986.

No other spacecraft has ever visited the Uranian system or Oberon, and no mission is planned in the foreseeable future.

2nd Largest Moon of Saturn - Rhea (20th Moon outwards from Saturn)

Rhea is the second largest moon of Saturn and the nineth largest moon in the Solar System.

Discovery

It was discovered in 1672 by Giovanni Domenico Cassini. Cassini named the four moons he discovered (Tethys, Dione, Rhea and Iapetus) Sidera Lodoicea (the stars of Louis) to honor King Louis XIV.

Naming

Rhea is named after the Titan Rhea of Greek mythology.

Rhea was the Titaness daughter of Uranus, the sky, and Gaia, the earth, in Greek mythology. She was known as "the mother of gods". In earlier traditions, she was strongly associated with Gaia and Cybele, the Great Goddess, and was later seen by the classical Greeks as the mother of the Olympian gods and goddesses, though never dwelling permanently among them on Mount Olympus.

Stats

Diameter: 1,527 km

Semi-major axis: 527,108 km

Orbital Period: 4.52 days

Orbit

Rhea takes as long to rotate on its axis as it does to make one orbit of Saturn; and therefore always keeps the same hemisphere pointed to Saturn.

Possible ring system?

On March 6, 2008, NASA announced that Rhea may have a tenuous ring system. This would mark the first discovery of rings about a moon. The rings' existence was inferred by observed changes in the flow of electrons trapped by Saturn's magnetic field as Cassini passed by Rhea.

Dust and debris could extend out to Rhea's Hill sphere, but were thought to be denser nearer the moon, with three narrow rings of higher density. The case for a ring was strengthened by the subsequent finding of the presence of a set of small ultraviolet-bright spots distributed along Rhea's equator (interpreted as the impact points of deorbiting ring material).

However, when Cassini made targeted observations of the putative ring plane from several angles, no evidence of ring material was found, suggesting that another explanation for the earlier observations is needed.

Surface features

Rhea has a rather typical heavily cratered surface, with the exceptions of a few large fractures (wispy terrain) on the trailing hemisphere (the side facing away from the direction of motion along Rhea's orbit) and a very faint "line" of material at Rhea's equator that may have been deposited by material deorbiting from its rings.

Its surface can be divided into two geologically different areas based on crater density. The first area contains craters which are larger than 40 km in diameter. The second area, in parts of the polar and equatorial regions, has only craters under that size. This suggests that a major resurfacing event occurred some time during its formation.

Atmosphere

On November 27, 2010, NASA announced the discovery of a tenuous atmosphere—exosphere. It consists of oxygen and carbon dioxide in proportion of roughly 5 to 2.

The surface density of the exosphere is from 105 to 106 molecules in a cubic centimeter depending on local temperature. The main source of oxygen is radiolysis of water ice at the surface by ions supplied by the magnetosphere of Saturn. The source of the carbon dioxide is less clear, but it may be related to oxidation of the organics present in ice or to outgassing of the moon's interior.

Life?

Models suggest that Rhea could be capable of sustaining an internal liquid water ocean through heating by radioactive decay.

If there are thermal vents on the floor of this ocean as there are on Earth, it is remotely possible that similar organisms to those which live around the vents on Earth could also survive there.

2nd Largest Moon of Jupiter - Callisto (8th Moon outwards from Jupiter)

Callisto is the third-largest moon in the Solar System and the second largest in the Jovian system.

Discovery

Callisto's discovery is credited to Galileo Galilei, who was the first to observe it on January 7, 1610.

The satellite's name was soon suggested by astronomer Simon Marius. Callisto is named after one of Zeus's many lovers in Greek mythology. Callisto was a nymph (or, according to some sources, the daughter of Lycaon) who was associated with the goddess of the hunt, Artemis.

Together with Ganymede, Io and Europa, they are collectively known as Galilean satellites after the discover.

Stats

Diameter: 4,821 km

Semi-major axis: 1,882,709 km

Orbital Period: 16.69 days

Orbits

Callisto is the outermost of the four Galilean moons of Jupiter. It orbits at a distance of 1,882,709 km. This is significantly larger than the orbital radius —1,070,412 km— of the next-closest Galilean satellite, Ganymede. As a result of this relatively distant orbit, Callisto does not participate in the mean-motion resonance in which the three inner Galilean satellites are locked.

Callisto rotates synchronously with its orbital period, so the same hemisphere always faces (is tidally locked to) Jupiter. Callisto's surface is less affected by Jupiter's magnetosphere than the other inner satellites because it orbits farther away, and thus does not experience appreciable tidal heating.

Composition

Callisto is composed of approximately equal amounts of rock and ices. Compounds detected spectroscopically on the surface include water ice, carbon dioxide, silicates, and organic compounds. Investigation by the Galileo spacecraft revealed that Callisto may have a small silicate core and possibly a subsurface ocean of liquid water at depths greater than 100 km.

The surface of Callisto is heavily cratered and extremely old. It does not show any signatures of subsurface processes such as plate tectonics or volcanism, and is thought to have evolved predominantly under the influence of impacts.

Atmosphere

Callisto is surrounded by an extremely thin atmosphere composed of carbon dioxide and probably molecular oxygen, as well as by a rather intense ionosphere.

Life?

There is a distinct possibility that Callisto's saltwater ocean could harbour life. If there are thermal vents on the floor of this saltwater ocean as there are on Earth, it is remotely possible that similar organisms to those which live around the vents on Earth could also survive there.

Life has less chance at Callisto than at Europa and Ganymede, because Callisto orbits further away from Jupiter and lack the tidal heat energy.

Quasi-satellite of Venus - Asteroid 2002 VE68

A quasi-satellite is an object in a 1:1 orbital resonance with its planet that stays close to the planet over many orbital periods.

A quasi-satellite's orbit around the Sun takes exactly the same time as the planet's, but has a different eccentricity (usually greater). When viewed from the perspective of the planet, the quasi-satellite will appear to travel in an oblong retrograde loop around the planet.

In contrast to true satellites, quasi-satellite orbits lie outside the planet's Hill sphere, and are unstable. Over time they tend to evolve to other types of resonant motion, where they no longer remain in the planet's neighbourhood, then possibly later move back to a quasi-satellite orbit, etc.

Asteroid 2002 VE68 is a quasi-satellite of Venus. It was discovered on November 11, 2002, by Lowell Observatory Near-Earth-Object Search (LONEOS).

Stats

Asteroid Family Group: Aten asteroid

Diameter: 210 - 470 m

Semi-major axis: 0.724 AU (same as Venus)

Rotation: 13.5 hours


The asteroid 2002 VE68 is currently a quasi-satellite of Venus, the first object of this dynamical class to be discovered, and is also the first known co-orbital companion to Venus.

This asteroid is also a Mercury grazer and an Earth crosser; it seems to have been co-orbital with Venus for only the last 7000 years, and is destined to be ejected from this orbital arrangement about 500 years from now. During this time, its distance to Venus has been and will remain larger than about 0.2 AU.

It has a high eccentricity (~ 0.4) and inclination (~ 9°). Consequently the maximum distance of the asteroid from the Sun is near that of the Earth and the minimum distance is smaller than the aphelion of Mercury.

From the evolution of the orbit of this object, it may have been a near-Earth asteroid, which, some 7000 yr ago, was injected into its present orbit by the action of the Earth.

Ceres - Largest asteroid, Smallest dwarf planet

Discovery

The idea that an undiscovered planet could exist between the orbits of Mars and Jupiter was first suggested by Johann Elert Bode in 1772.

His considerations were based on the Titius–Bode law, a now abandoned theory which had been first proposed by Johann Daniel Titius in 1766, observing that there was a regular pattern in the semi-major axes of the known planets marred only by the large gap between Mars and Jupiter. The pattern predicted that the missing planet ought to have a semi-major axis near 2.8 AU.

William Herschel's discovery of Uranus in 1781 near the predicted distance for the next body beyond Saturn increased faith in the law of Titius and Bode. In 1800, requests were sent to twenty-four experienced astronomers, asking that they combine their efforts and begin a methodical search for the expected planet.

One of the astronomers selected for the search was Giuseppe Piazzi at the Academy of Palermo, Sicily. Before receiving his invitation to join the group, Giuseppe Piazzi discovered Ceres on 1 January 1801. He was searching for "the 87th [star] of the Catalogue of the Zodiacal stars of Mr la Caille", but found that "it was preceded by another". Instead of a star, Piazzi had found a moving star-like object, which he first thought was a comet.

Naming

Piazzi originally suggested the name Cerere Ferdinandea for his discovery, after both the mythological figure Ceres (Roman goddess of agriculture) and King Ferdinand III of Sicily. "Ferdinandea" was not acceptable to other nations of the world and was thus dropped.

Stats

Diameter: 952 km
Semi-major axis: 2.766 AU
Orbital Period: 4.60 years
Rotation period: 9.07 hrs
Date discovered: 1801.1.1
Class: G
Type: Main-belt Asteroid

Status

The classification of Ceres has changed more than once. disagreement. Johann Elert Bode believed Ceres to be the "missing planet" he had proposed to exist between Mars and Jupiter, at a distance of 419 million km (2.8 AU) from the Sun. Ceres remained listed as a planet in astronomy books and tables (along with 2 Pallas, 3 Juno and 4 Vesta) for about half a century.

As other objects were discovered in the area it was realised that Ceres represented the first of a class of many similar bodies. In 1802 Sir William Herschel coined the term asteroid ("star-like") for such bodies, writing "they resemble small stars so much as hardly to be distinguished from them, even by very good telescopes". As the first such body to be discovered, it was given the designation "1 Ceres" under the modern system of asteroid numbering.

The 2006 debate surrounding Pluto and what constitutes a 'planet' led to Ceres being considered for reclassification as a planet. A proposal before the International Astronomical Union for the definition of a planet would have defined a planet as "a celestial body that:

(a) has sufficient mass for its self-gravity to overcome rigid-body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and
(b) is in orbit around a star, and is neither a star nor a satellite of a planet".

Had this resolution been adopted, it would have made Ceres the fifth planet in order from the Sun. It was not accepted, and in its place an alternate definition came into effect as of 24 August 2006, carrying the additional requirement that:

(c) a "planet" must have "cleared the neighborhood around its orbit".

By this definition, Ceres is not a planet because it does not dominate its orbit, sharing it as it does with the thousands of other asteroids in the asteroid belt and constituting only about a third of the total mass.

It is instead now classified as a dwarf planet.

Titius–Bode law - How Ceres was found

The Titius–Bode law (sometimes termed just Bode's law) is a hypothesis that the bodies in some orbital systems, including the Sun's, orbit at semi-major axes in a function of planetary sequence. The hypothesis correctly predicted the orbits of Ceres and Uranus, but failed as a predictor of Neptune's orbit.

The formula

The best way to see the law is to write down the sequence 0, 3, 6, 12 and so on, where each number is obtained by doubling its predecessor. Next, add 4 to each number, and divide the result by 10.

For example, Venus = (3+4)/10 = 0.7

Now get out any astronomy textbook and look up the distances of the planets from the Sun in astronomical units, the Earth-Sun distance being defined as 1. The distances are virtually identical to the terms in the number sequence for all but the outermost planets.

Planet   Titius–Bode law distance   Actual distance
Mercury            0.4                 0.39
Venus              0.7                 0.72
Earth              1.0                 1.0
Mars               1.6                 1.52
Ceres              2.8                 2.77
Jupiter            5.2                 5.2
Saturn            10.0                 9.74
Uranus            19.6                19.2
Neptune           38.8                30.06

When originally published, the law was approximately satisfied by all the known planets — Mercury through Saturn — with a gap between the fourth and fifth planets.

It was regarded as interesting, but of no great importance until the discovery of Uranus in 1781 which happens to fit neatly into the series.

Based on this discovery, Bode urged a search for a planet between Mars and Jupiter. Ceres, the largest object in the asteroid belt, was found at Bode's predicted position in 1801.

Bode's law was then widely accepted until Neptune was discovered in 1846 and found not to satisfy Bode's law.

Theoretical explanations

There is no solid theoretical explanation of the Titius–Bode law, but if there is one it is possibly a combination of orbital resonance and shortage of degrees of freedom: any stable planetary system has a high probability of satisfying a Titius–Bode-type relationship. Because of this, it has been called a "rule" rather than a "law".

Orbital resonance from major orbiting bodies creates regions around the Sun that are free of long-term stable orbits. Results from simulations of planetary formation support the idea that a randomly chosen stable planetary system will likely satisfy a Titius–Bode law.

Still, Titius–Bode law may be just a coincidence. And we really do not have other planetary systems to test it.

Asteroids

Asteroids are a class of small Solar System Bodies in orbit around the Sun. Asteroids are increasingly referred specifically to the small rocky–icy and metallic bodies of the inner Solar System out to the orbit of Jupiter.

There are millions of asteroids, many thought to be the often shattered remnants of planetesimals, bodies within the young Sun’s solar nebula that never grew large enough to become planets. A large majority of known asteroids orbit in the asteroid belt between the orbits of Mars and Jupiter or co-orbital with Jupiter.

Naming

A newly discovered asteroid is given a provisional designation (such as 2002 AT4) consisting of the year of discovery and an alphanumeric code indicating the half-month of discovery and the sequence within that half-month. Once an asteroid's orbit has been confirmed, it is given a number, and later may also be given a name.

Distribution within the Solar System

1. Asteroid belt

The majority of known asteroids orbit within the asteroid belt between the orbits of Mars and Jupiter, generally in relatively low-eccentricity (i.e., not very elongated) orbits. This belt is now estimated to contain between 1.1 and 1.9 million asteroids larger than 1 km in diameter, and millions of smaller ones. These asteroids may be remnants of a failed planet in the protoplanetary disk. In in this region the accretion of planetesimals into planets during the formative period of the Solar System was prevented by large gravitational perturbations by Jupiter.

2. Trojans

Trojan asteroids are a population that share an orbit with a larger planet or moon, but do not collide with it because they orbit in one of the two Lagrangian points of stability, L4 and L5, which lie 60° ahead of and behind the larger body.

The most significant population of Trojan asteroids are the Jupiter Trojans. A couple trojans have also been found orbiting with Mars.

3. Near-Earth asteroids

Near-Earth asteroids, or NEAs, are asteroids that have orbits that pass close to that of Earth. Asteroids that actually cross the Earth's orbital path are known as Earth-crossers. As of May 2010, 7,075 near-Earth asteroids are known and the number over one kilometre in diameter is estimated to be 500–1,000.

Quasi-satellites

Some asteroids have unusual horseshoe orbits that are co-orbital with the Earth or some other planet.

Sometimes these horseshoe objects temporarily become quasi-satellites for a few decades or a few hundred years, before returning to their earlier status. Both Earth and Venus are known to have quasi-satellites.

Largest Moon of Uranus - Titania (17th Moon outwards from Uranus)

Uranus has 27 known moons, all of which are named after characters from the works of William Shakespeare and Alexander Pope.

Titania is the largest of the moons of Uranus and the eighth largest moon in the Solar System

Discovery

Titania was spotted by Sir William Herschel on January 11, 1787, six years after he had discovered the planet itself.



Naming

The responsibility for naming was taken by John Herschel, son of the discoverer of Uranus. Herschel, instead of assigning names from Greek mythology, named the moons after magical spirits in English literature. Titania is named after the queen of the fairies in Shakespeare's A Midsummer Night's Dream.

Stats

Diameter: 1,577 km

Semi-major axis: 435,910 km

Orbital Period: 8.71 days

Orbit

Titania orbits Uranus at the distance of about 436,000 km, being the second farthest from the planet among its five major moons. Its orbital period is around 8.7 days, coincident with its rotational period. In other words, Titania is a synchronous or tidally locked satellite, with one face always pointing toward the planet.

Formation

Titania probably formed from an accretion disk that surrounded the planet just after its formation.

Titania consists of approximately equal amounts of ice and rock, and is likely differentiated into a rocky core and an icy mantle. A layer of liquid water may be present at the core–mantle boundary. The surface of Titania, which is relatively dark and slightly red in color, appears to have been shaped by both impacts and endogenic processes.

Atmosphere

The presence of carbon dioxide on the surface suggests that Titania may have a tenuous seasonal atmosphere of CO2. Other gases like nitrogen or methane are unlikely to be present, because the moon's weak gravity could not prevent them escaping into the space.

Exploration Status

So far the only close-up images of Titania have been from the Voyager 2 probe, which photographed the moon during its flyby of Uranus in January 1986.

No other spacecraft has ever visited the Uranian system or Titania, and no mission is planned in the foreseeable future.

Largest Moon of Neptune - Triton (7th Moon outwards from Neptune)

Discovery

Neptune has thirteen known moons. The largest of which is Triton, discovered by William Lassell on October 10, 1846, just 17 days after the discovery of Neptune itself.

Naming
Triton is named after the Greek sea god Triton, the son of Poseidon (the Greek god comparable to the Roman Neptune). The name was first proposed by Camille Flammarion in his 1880 book Astronomie Populaire, but it did not come into common use until at least the 1930s.


Voyager 2 photomosaic of Triton's sub-Neptunian hemisphere.



Triton is the only large moon in the Solar System with a retrograde orbit, which is an orbit in the opposite direction to its planet's rotation.

Stats

Diameter: 2,705 km

Semi-major axis: 354,759 km

Orbital Period: 5.88 days

Triton is the seventh largest moon in the Solar System, and is larger than the dwarf planets Pluto and Eris. Because of its retrograde orbit and composition similar to Pluto's, it is thought to have been captured from the Kuiper belt.

Capture from Kuiper belt

The proposed capture of Triton may explain several features of the Neptunian system, including the extremely eccentric orbit of Neptune's moon Nereid and the scarcity of moons as compared to the other gas giants.

Triton's initially eccentric orbit would have intersected orbits of irregular moons and disrupted those of smaller regular moons, dispersing them through gravitational interactions.

Two types of mechanisms have been proposed for Triton's capture.

In order to be gravitationally captured by a planet, a passing body must lose sufficient energy to be slowed down to a speed less than that required to escape. An early theory of how Triton may have been slowed was by collision with another object, either one that happened to be passing by Neptune (which is unlikely), or a moon or proto-moon in orbit around Neptune (which is more likely).

A more recent and now favored hypothesis suggests that, before its capture, Triton had a massive companion similar to Pluto's moon Charon with which it formed a binary. When the binary encountered Neptune, it interacted in such a way that orbital energy was transferred from Triton to its companion; the latter was expelled, while Triton became bound to Neptune.

This hypothesis is supported by several lines of evidence, including binaries being very common among the large Kuiper belt objects. The event was brief but gentle, saving Triton from collisional disruption. Events like this may have been common during the formation of Neptune, or later when it migrated outward.

Orbit

Triton takes as long to rotate on its axis as it does to make one orbit of Neptune; and therefore always keeps the same hemisphere pointed to Neptune.

Atmosphere

Triton has a surface of mostly frozen nitrogen, a mostly water ice crust, an icy mantle and a substantial core of rock and metal.

Triton is one of the few moons in the Solar System known to be geologically active. As a consequence, its surface is relatively young and has relatively few impact craters, with a complex geological history revealed in intricate and mysterious cryovolcanic and tectonic terrains. Part of its crust is dotted with geysers believed to erupt nitrogen.

Triton has a tenuous nitrogen atmosphere, with trace amounts of carbon monoxide and small amounts of methane near the surface. Like Pluto's atmosphere, the atmosphere of Triton is believed to have resulted from evaporation of nitrogen from the moon's surface.

The surface temperature is at least −237.6 °C because Triton's nitrogen ice is in the warmer, hexagonal crystalline state, and the phase transition between hexagonal and cubic nitrogen ice occurs at that temperature.

Largest Moon of Saturn - Titan (21st Moon outwards from Saturn)

Discovery

Titan was discovered in 1655 by Christiaan Huygens using a 57-millimeter objective lens on a refracting telescope of his own design.

Naming

The name Titan, and the names of all seven satellites of Saturn then known, come from John Herschel (son of William Herschel, discoverer of Mimas and Enceladus) in his 1847 publication Results of Astronomical Observations Made at the Cape of Good Hope. He suggested the names of the mythological Titans, sisters and brothers of Kronos, the Greek Saturn.

Stats

Titan is frequently described as a planet-like moon. Titan has a diameter roughly 50% larger than Earth's moon and is 80% more massive. It is the second-largest moon in the Solar System, after Jupiter's moon Ganymede, and it is larger by volume than the smallest planet, Mercury.

Diameter: 5,151 km

Semi-major axis: 1,221,930 km

Orbital Period: 15.95 days

Orbit

Titan takes as long to rotate on its axis as it does to make one orbit of Saturn; and therefore always keeps the same hemisphere pointed to Saturn.

Composition

Titan is primarily composed of water ice and rocky material. Much as with Venus prior to the Space Age, the dense, opaque atmosphere prevented understanding of Titan's surface until new information accumulated with the arrival of the Cassini–Huygens mission in 2004.

This includes the discovery of liquid hydrocarbon lakes in the satellite's polar regions. These are the only large, stable bodies of surface liquid known to exist anywhere other than Earth. The surface is geologically young; although mountains and several possible cryovolcanoes have been discovered, it is smooth and few impact craters have been discovered.

Atmosphere

The atmosphere of Titan is largely composed of nitrogen; minor components lead to the formation of methane and ethane clouds and nitrogen-rich organic smog. The climate — including wind and rain — creates surface features similar to those of Earth, such as sand dunes, rivers, lakes and seas (probably of liquid methane or ethane) and shorelines, and, like on Earth, is dominated by seasonal weather patterns.

Life?

With its liquids (both surface and subsurface) and robust nitrogen atmosphere, Titan is viewed as analogous to the early Earth, although at a much lower temperature.

The satellite has thus been cited as a possible host for microbial extraterrestrial life or, at least, as a prebiotic environment rich in complex organic chemistry. Researchers have suggested a possible underground liquid ocean might serve as a biotic environment.

It has also been suggested that a form of life may exist on the surface, using liquid methane as a medium instead of water; and anomalies in atmospheric composition have been reported which are consistent with the presence of such a life-form, but which could also be due to an exotic non-living chemistry.

Largest Moon in the Solar System - Ganymede (7th Moon outwards from Jupiter)

Discovery

Ganymede's discovery is credited to Galileo Galilei, who was the first to observe it on January 7, 1610. The satellite's name was soon suggested by astronomer Simon Marius, for the mythological Ganymede, cupbearer of the Greek gods and Zeus's lover.

Together with Io, Europa and Callisto, they are collectively known as Galilean satellites after the discover.





Stats

Ganymede is the largest moon in the Solar System and it is even 8% larger than that the planet Mercury. It also has the highest mass of all planetary satellites, with 2.02 times the mass of the Earth's moon.

Diameter: 5,262 km

Semi-major axis: 1,070,412 km

Orbital Period: 7.15 days

Ganymede completes an orbit in roughly seven days and participates in a 1:2:4 orbital resonance with the moons Europa and Io, respectively.

Ganymede takes as long to rotate on its axis as it does to make one orbit of Jupiter; and therefore always keeps the same hemisphere pointed to Jupiter.

Composition

Ganymede is composed of approximately equal amounts of silicate rock and water ice. It is a fully differentiated body with an iron-rich, liquid core. A saltwater ocean is believed to exist nearly 200 km below Ganymede's surface, sandwiched between layers of ice.

Its surface is composed of two main types of terrain. Dark regions, saturated with impact craters and dated to four billion years ago, cover about a third of the satellite. Lighter regions, crosscut by extensive grooves and ridges and only slightly less ancient, cover the remainder. The cause of the light terrain's disrupted geology is not fully known, but was likely the result of tectonic activity brought about by tidal heating.

Ganymede is the only satellite in the Solar System known to possess a magnetosphere, likely created through convection within the liquid iron core. The meager magnetosphere is buried within Jupiter's much larger magnetic field and connected to it through open field lines.

Atmosphere

Ganymede also has a thin oxygen atmosphere that includes O, O2, and possibly O3 (ozone). Atomic hydrogen is a minor atmospheric constituent. Whether the satellite has an ionosphere associated with its atmosphere is unresolved.

Life?

There is a distinct possibility that Ganymede's saltwater ocean could harbour life. If there are thermal vents on the floor of this saltwater ocean as there are on Earth, it is remotely possible that similar organisms to those which live around the vents on Earth could also survive there.

But because of the depth of the saltwater ocean (possibly 200 km) from the surface of Ganymede, we may never know whether life exist there.

Moons of Mars - Phobos and Deimos

Mars has two small moons, Phobos and Deimos, which are thought to be captured asteroids. Both satellites were discovered in 1877 by Asaph Hall, and are named after the characters Phobos (panic/fear) and Deimos (terror/dread) who, in Greek mythology, accompanied their father Ares, god of war, into battle. Ares was known as Mars to the Romans.

Color image of Phobos obtained by Mars Reconnaissance Orbiter on March 23, 2008.

Diameter: 22.2 km (27×21.6×18.8)

Semi-major axis: 9377 km

Orbital period: 7.66 h

Color image of Deimos taken by the Mars Reconnaissance Orbiter on February 21, 2009.

Diameter: 12.6 km (10×12×16)

Semi-major axis: 23 460 km

Orbital period: 30.35 h



Origin

The origin of the Martian moons is still controversial. Phobos and Deimos both have much in common with carbonaceous C-type asteroids, with spectra, albedo, and density very similar to those of C- or D-type asteroids. Based on their similarity, one hypothesis is that both moons may be captured main-belt asteroids.

Both moons have very circular orbits which lie almost exactly in Mars's equatorial plane, and hence a capture origin requires a mechanism for circularizing the initially highly eccentric orbit, and adjusting its inclination into the equatorial plane, most probably by a combination of atmospheric drag and tidal forces, although it is not clear that sufficient time is available for this to occur for Deimos.

Capture also requires dissipation of energy. The current Mars atmosphere is too thin to capture a Phobos-sized object by atmospheric braking. Geoffrey Landis has pointed out that the capture could have occurred if the original body was a binary asteroid that separated under tidal forces.

Phobos could be a second-generation Solar System object that coalesced in orbit after Mars formed, rather than forming concurrently out of the same birth cloud as Mars.

Another hypothesis is that Phobos and Deimos were formed by ejected materials, after a collision between Mars with a large planetesimal, similar to the prevailing theory for the origin of Earth's moon.

Observations of Phobos in the thermal infrared suggest a composition containing mainly phyllosilicates, which are well known from the surface of Mars.