recursal/Fanatic-Fandom huggingface dataset:
Daphnis

**Daphnis** is an inner satellite of Saturn. It is also known as Saturn XXXV or its provisional

## Daphnis

Daphnis and its equatorial ridge as seen by Cassini

## Physical Characteristics

### Mean Surface Gravity

0.0002 m/s² at longest axisto 0.0006 m/s² at poles

### Mean Escape Velocity

0.001 km/s at longest axisto 0.002 km/s at poles

### Albedo (Geometric)

~0.5

designation, S/2005 S 1. Daphnis is about 8 kilometers in diameter and orbits Saturn in the Keeler Gap within the A Ring.

## Naming

The moon was named in 2006 after Daphnis, a shepherd, pipes player, and pastoral poet in Greek mythology; he was descendant of the Titans, after whom the largest moons of Saturn are named. Both Daphnis and Pan, the only other known shepherd moon to orbit within Saturn's main rings, are named for mythological figures associated with shepherds.

## Orbit

The inclination and eccentricity of Daphnis's orbit are very small, but distinguishable from zero. Both, particularly the inclination, are significantly greater than those of Pan (the larger moonlet which forms the Encke Gap). Daphnis's eccentricity causes its distance from Saturn to vary by ~9 km, and its inclination causes it to move up and down by ~17 km. The Keeler Gap, within which Daphnis orbits, is about 42 km wide.

## Physical Characteristics

On January 18, 2017, Daphnis was photographed from a sufficiently close distance to reveal its shape. The moon was discovered to be an irregularly-shaped object with a mostly smooth surface, a few craters, and an equatorial ridge, similar to some other shepherd moons of Saturn like Atlas and Pan.
Amalthea (disambiguation)

***This article is a disambiguation page for Amalthea (disambiguation)***
**The following is a list of links to pages that might share the same title.**
Please follow one of the disambiguation links below or use the search tool to find the page you were looking for if it is not listed. If an internal link led you here, you may wish to change the link to point directly to the intended article.,

Amalthea may refer to:

• Amalthea (moon), a moon of Jupiter.
• 113 Amalthea, an asteroid in the asteroid belt.
Gallic group

The Gallic group is a collection of prograde irregular moons of Saturn containing 7 members having a semi-major axis between 16 million kilometers and 19 million kilometers, eccentricity around 0.53 and inclination between 35° and 40° along with 2 other moons that is more distant. Albiorix is the largest among the Gallic group with a diameter of about 29 kilometers, followed by Tarvos being the 2nd at 16 kilometers and Erriapus being the 3rd at 12 kilometers.
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Halimede

**Halimede**, or **Neptune IX**, is a retrograde irregular satellite of Neptune. It was discovered by Matthew J. Holman, John J. Kavelaars, Tommy Grav, Wesley C. Fraser and Dan Milisavljevic on August 14, 2002.

## Halimede

Halimede imaged by Very Large Telescope in September 3, 2002 during its follow-up observations

## Physical Characteristics

### Diameter

62 km

Halimede is the 2nd closest retrograde irregular moon of Neptune after Triton, the largest and the closest.
Project/Paraphrase2

Project #3

**Project Paraphrase2 aims to help reduce the number of pages that have been copied and pasted from other sites. As a reminder, Project/Paraphrase2 is a continuation of Project/Paraphrase. The projects aims to improve, add links and formatting, fix spelling errors in pages marked with this header:**

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The guidelines are as follows.

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Jarnsaxa

**Jarnsaxa**, also known as **Saturn L** (provisional designation **S/2006 S 6**), is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on June 26, 2006, from observations taken between January 5 and April 29, 2006.

## Physical Characteristics

### Mean Radius

3 km

Jarnsaxa is about ~6 kilometres in diameter, and orbits Saturn at an average distance of 18,556.9 Mm in 943.784 days, at an inclination of 162.9° to the ecliptic, in a retrograde direction and with an eccentricity of 0.1918. Jarnsaxa is a member of the Norse group, a large collection of retrograde irregular natural satellites of Saturn that orbits in the opposite direction from its rotation.
Pandia

**Pandia**, also designated **Jupiter LXV**, is a small prograde outer natural satellite of Jupiter discovered by Scott S. Sheppard on 11 May 2018. It was announced along with other 9 other moons on 17 July 2018 and it provisionally designated **S/2017 J 4**.

## Pandia

Precovery image of Pandia taken by Canada-France-Hawaii Telescope oin February 28, 2003

## Physical Characteristics

### Diameter

3 km

Pandia belongs to the Himalia group, a collection of prograde irregular natural satellites that orbits the same direction as Jupiter's rotation. It has precovery images dated back in February 28, 2003.
Aoede

**Aoede**, also known as **Jupiter XLI**, is an irregular natural satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2003. It was given its provisional designation **S/2003 J 7**.

## Physical Characteristics

### Diameter

4 km

Aoede is about ~4 kilometres in diameter, and orbits Jupiter at an average distance of 23,044,000 km in 714.657 days in the retrograde direction, at an inclination of 160° to the ecliptic, in a retrograde direction and with an eccentricity of 0.4311.

Aoede belongs to the Pasiphae group, a group of irregular moons orbiting Jupiter in the opposite direction from its rotation.
S/2004 S 29

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**Saturn LX**, provisionally known as **S/2004 S 29**, is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, and Jan Kleyna on October 7, 2019 from observations taken between December 12, 2004 and January 17, 2007.

## Designations

### Alternative Names

Saturn LX
S2428b

## Physical Characteristics

### Diameter

4 km

It was given its permanent designation **Saturn LX** in August 2021. S/2004 S 29 was a member of the Inuit group in 2019 and was recategorized to the Gallic group in 2022, since the inclination is less inclined than the Inuit group. As of 2023, it has not given its official name.

Saturn LX is about ~4 kilometres in diameter, and orbits Saturn at an average distance of 17 million km in 837.78 d, at an average inclination of 38.6° to the ecliptic, with an eccentricity of 0.485.
Despina

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**Despina**, also known as **Neptune V**, is the third-closest inner moon of Neptune.

## Discovery

### Discovered by

Stephen P. Synnott
Voyager Imaging Team

## Physical Characteristics

### Mean Density

~1.2 g/cm³

It was given its provisional designation **S/1989 N 3** after the discovery.
Carpo

**Carpo**, also **Jupiter XLVI** is a very inclined small outer natural satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2003, and was given its provisional designation **S/2003 J 20**.

## Carpo

Image of Carpo by Canada-France-Hawaii Telescope on February 25, 2003

## Physical Characteristics

### Diameter

3 km

Carpo has a diameter of about ~3 km. On average, Carpo's orbit has a semi-major axis of 17 million km, a high eccentricity of 0.42, and a very high inclination of 54° with respect to the ecliptic.

Carpo was once orbits alone (an outlier) like Themisto and Valetudo, until S/2018 J 4 was announced in January 20, 2023.
Phobos

**This page/section has been marked for fixing under Project/Paraphrase**
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This article is a stub — it needs more information. You can help Solarpedia by expanding it.

***Phobos*** is the larger, inner of **Mars**' two moons and is 17 x 14 x 11 miles (27 by 22 by 18 kilometers) in diameter. It orbits Mars three times a day, and is so close to the planet's surface that in some locations on Mars it cannot always be seen.
S/2007 S 3

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**S/2007 S 3** is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 1 May 2007 from observations taken between 18 January and 19 April 2007.

## Physical Characteristics

### Diameter

5 km

S/2007 S 3 is about ~5 kilometres in diameter, and orbits Saturn at an average distance of 19,429,000 kilometres in about 1,011 days, at an inclination of 176.6° to the ecliptic, in a retrograde direction and with an eccentricity of 0.143.

S/2007 S 3 was considered lost after its discovery and was then recovered in October 12, 2022.
Hati

**Hati** or **Saturn XLIII** is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 4 May 2005, from observations taken between 12 December 2004 and 11 March 2005.

## Hati

Image of Hati taken by Cassini in November 2015

## Physical Characteristics

### Synodic Rotation Period

5.45 h

Hati is about ~6 kilometers in diameter, and orbits Saturn at an average distance of 20,303 Mm in 1039 days, at an inclination of 163° to the ecliptic (165° to Saturn's equator), in a retrograde direction and with an eccentricity of 0.291, nearly the same as the orbit of its member in the Norse group, Mundilfari.
S/2006 S 12

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**S/2006 S 12** is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, E. Ashton and Brett J. Gladman on May 7, 2023 from observations taken between January 5, 2006 and July 8, 2021.

## Physical Characteristics

### Diameter

4 km

S/2006 S 12 is about ~4 kilometers in diameter, and orbits Saturn at a distance of 19.569 Gm in 1,043.16 days, at an inclination of 39.03, orbits in prograde direction and eccentricity of 0.542.

S/2006 S 12 belongs to the Gallic group. However, its semi-major axis is barely further, meaning it is an outlier, just like S/2004 S 24.
S/2004 S 28

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**S/2004 S 28** is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, and Jan Kleyna on October 7, 2019 from observations taken between December 12, 2004 and March 21, 2007.

## Physical Characteristics

### Mean Radius

2 km

S/2004 S 28 is about ~4 kilometres in diameter, and orbits Saturn at an average distance of 22.020 Gm in 1220.31 days, at an inclination of 170° to the ecliptic, in a retrograde direction and with an eccentricity of 0.143.
S/2015 (136472) 1

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## S/2015 (136472) 1

Makemake and its moon imaged by Hubble Space Telescope

## Discovery

### Discovered by

HST/Wide Field Camera 3
Alex H. Parker
Marc W. Buie
William M. Grundy
Keith S. Noll

## Orbit Data

### Satellite of

Makemake

**S/2015 (136472) 1**, nicknamed **MK2** by the discovery team, is the only known moon of the trans-Neptunian dwarf planet Makemake. It is estimated to be 175 km (110 mi) in diameter (for an assumed albedo of 4%) and has a semi-major axis at least 21,000 km (13,000 mi) from Makemake. Its orbital period is ≥ 12 days (the minimum values are those for a circular orbit; the actual orbital eccentricity is unknown). Observations leading to its discovery occurred in April 2015, using the *Hubble Space Telescope*'s Wide Field Camera 3, and its discovery was announced on 26 April 2016.

Makemake and Sedna are the least-well-known of the large trans-Neptunian objects. The discovery of MK2 and follow-up observations in 2018 will enable Makemake's mass to be determined, which will allow an estimate of its density and other characteristics.
Janus

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**Janus** is an inner satellite of Saturn. It is also known as **Saturn X.**

## History

### Discovery

Janus was identified by Audouin Dollfus on 15 December 1966 and given the temporary designation **S/1966 S 2**. Previously, Jean Texereau had photographed Janus on 29 October 1966 without realising it. On 18 December, Richard Walker observed an object in the same orbit as Janus, but whose position could not be reconciled with the previous observations. Twelve years later, in October 1978, Stephen M. Larson and John W. Fountain realised that the 1966 observations were best explained by two distinct objects (Janus and Epimetheus) sharing very similar orbits, Walker is now credited with the discovery of Epimetheus. *Voyager 1* confirmed this orbital configuration in 1980. (See co-orbital moon for a more detailed description of their unique arrangement.)
Siarnaq

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**Siarnaq**, also designated **Saturn XXIX**, is the second-largest irregular moon of Saturn. It was discovered on 23 September 2000 by a team of astronomers led by Brett J. Gladman.

## Siarnaq

Images of Siarnaq taken by Canada-France-Hawaii Telescope in September 2000

## Designations

### Adjectives

Siarnaupian
Siarnaqian

## Physical Characteristics

### Synodic Rotation Period

10.18785 h

Siarnaq is the largest member of both Inuit group and its own subgroup. Its subgroup contains: Itself, Tarqeq, S/2004 S 31, S/2019 S 6, S/2019 S 14 and S/2020 S 5.
Tarvos

**Tarvos**, or **Saturn XXI**, is a prograde irregular satellite of Saturn. It was discovered by John J. Kavelaars et al. on September 23, 2000, and given its provisional designation **S/2000 S 4**.

## Tarvos

Images of Tarvos taken by Canada-France-Hawaii Telescope in September 2000

## Physical Characteristics

### Synodic Rotation Period

10.691 h

Tarvos is the first prograde irregular natural satellite discovered that belongs to the Gallic Group. Tarvos could be a fragment that broke off the largest moon of the Gallic group, Albiorix.
Callirrhoe

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**Callirrhoe**, also known as **Jupiter XVII**, is Jupiter's retrograde irregular natural satellites. It was imaged by Spacewatch at Kitt Peak National Observatory from October 6 through November 4, 1999.

## Callirrhoe

Callirrhoe imaged by LORRI instrument aboard New Horizons

## Physical Characteristics

### Diameter

9.6 ± 1.3km

Callirrhoe is about ~9 kilometers in diameter. Callirrhoe was thought to be an asteroid (designated as **1998 UX₁₈**) until it was confirmed to be a moon and given its provisional designation **S/1999 J 1**.
Norse group

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The Norse group is a huge collection of retrograde irregular moons of Saturn consisting of 100 known members having a semi-major axis between 12 million kilometers and 26 million kilometers, eccentricity between 0.13 and 0.77, and inclination between 136° and 178°. As of November 2023, it was the first moon group to have reached 100 members. Like the Inuit group, the Norse group has subgroups but only 3 of them are confirmed so far.
Neso

**Neso**, also known as **Neptune XIII**, is the outermost known natural satellite of Neptune. It's a retrograde irregular moon discovered by Matthew J. Holman, Brett J. Gladman, et al. on 14 August 2002.

## Neso

Images of Neso taken by Very Large Telescope's FORS1 imager in September 2002

## Designations

### Adjectives

Nesoan
Nesoian

## Physical Characteristics

### Diameter

60 km

Neso is about ~60 km in diameter based on an assumed albedo.

Given the similar orbital elements with Psamathe, it was suggested that both irregular satellites could have been a fragment piece of a much bigger moon in the past.

Neso's furthest point is much further than the distance between the Sun and Mercury.
Moai

**Moai** or **moʻai** (/ˈmoʊ.aɪ/ (listen) *MOH-eye*; Spanish: *moái*; Rapa Nui: *moʻai*, lit. 'statue') are monolithic human figures carved by the Rapa Nui people on Rapa Nui (Easter Island) in eastern Polynesia between the years 1250 and 1500. Nearly half are still at Rano Raraku, the main moai quarry, but hundreds were transported from there and set on stone platforms called ahu around the island's perimeter. Almost all moai have overly large heads, which comprise three-eighths the size of the whole statue and they have no legs. The moai are chiefly the living faces (*aringa ora*) of deified ancestors (*aringa ora ata tepuna*). The statues still gazed inland across their clan lands when Europeans first visited the island in 1722, but all of them had fallen by the latter part of the 19th century. The moai were toppled in the late 18th and early 19th centuries, possibly as a result of European contact or internecine tribal wars.

The production and transportation of the more than 900 statues is considered a remarkable creative and physical feat. The tallest moai erected, called *Paro*, was almost 10 metres (33 ft) high and weighed 82 tonnes (81 long tons; 90 short tons). The heaviest moai erected was a shorter but squatter moai at Ahu Tongariki, weighing 86 tonnes (85 long tons; 95 short tons). One unfinished sculpture, if completed, would be approximately 21 m (69 ft) tall, with a weight of about 145–165 tonnes (143–162 long tons; 160–182 short tons). Statues are still being discovered as of 2023.
S/2003 J 19

**Jupiter LXI**, provisionally known as **S/2003 J 19**, is a natural satellite of Jupiter. It was discovered by a team of astronomers led by Brett J. Gladman, et al. in 2003.

## Physical Characteristics

### Diameter

2 km

S/2003 J 19 is about ~2 kilometres in diameter, and orbits Jupiter at an average distance of 22,709 Mm in 699.125 days, at an inclination of 165° to the ecliptic, in a retrograde direction and with an eccentricity of 0.1961.

S/2003 J 19 was considered lost after its discovery in 2003 and was recovered in 2018 along then given its permanent designation. As of 2023, it was not given its official name.

S/2003 J 19 belongs to the Carme group, made up of irregular retrograde moons orbiting Jupiter in the opposite direction.
S/2018 J 2

**S/2018 J 2** is a very small outer irregular moon of Jupiter in the Himalia Group. It’s the most recently discovered natural satellite in its group, only being discovered in May of 2018. Very little is known about it due to how recently discovered it was.

## Discovery

S/2018 J 2 was discovered when Scott S. Sheppard was using the 13.1-foot Víctor M. Blanco telescope in Chile. It was discovered on May 12, 2018. Despite being discovered in 2018, it wasn’t until December of 2022 Walter various observations were made to confirm the satellite’s orbit and existence. It was announced along with S/2011 J 3.

## Appearance & Size

It’s not known what S/2018 J 2 looks like, but it may look similar to other Himalia group moons, and may be light gray and color. Not much else can be inferred about its appearance due to a lack of information about it. S/2018 J 2 is estimated to be 1.86 miles in diameter, making it amongst the smallest moons in the Himalia Group.

## Orbit

The semi-major axis of S/2018 J 2 is 7.1 million miles, and it has an orbit eccentricity of 0.11841. It also has an inclination of 28.6592°. This makes its orbit similar to other Himalia Group moons, and it also takes 250.88 days to finish an orbit. This makes it the overall 12th closest moon to Jupiter.
6Q0B44E

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**This object is a temporary satellite of: Earth**
It may or may still be in Earth orbit. **This object is/might be not natural**
It may be of artificial origin and may not have formed naturally
**6Q0B44E**, sometimes abbreviated to **B44E**, is a small object or probably an item of space debris, that is currently orbiting **Earth** outside the orbit of the **Moon** as of November 2018.

## Discovery

6Q0B44E was first observed by Catalina Sky Survey researchers at the Lunar and Planetary Laboratory of the University of Arizona on 28 August 2006. The sighting was confirmed the next day by observations at the Siding Spring Survey and Table Mountain Observatory.

## Observations

6Q0B44E was spotted at what was later calculated to be the brightest part of its orbit, at 19th magnitude. As the object moved away from Earth, its brightness dropped on an approximately six-month cycle down to 28th magnitude, severely limiting study.

The object was observed 56 times in the seven months after its discovery, but was lost in March 2007. Another unidentified satellite of Earth, XL8D89E, was discovered in June 2016 on a similar - but not identical - orbit. It is likely, though unproven, that both 6Q0B44E and XL8D89E are the same object, with the orbit shifted in the intervening decade by non-gravitational accelerations (such as slow escape of gas).
Proteus

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Proteus is the second largest Neptunian moon discovered by the Voyager 2 spacecraft. It’s name Proteus was named after Proteus the Greek God.

## Orbit Data

### Inclination

0.524° (to Neptune's equator)
0.026°±0.007° (to local Laplace plane)

## Physical Characteristics

### Mean Surface Temperature

≈ 51 K mean (estimate)

Proteus orbits Neptune at 4.75 times Neptune's equator.

### Discovery

Bradford A. Smith announced the discovery on July 7, 1989. On September 16, 1991 S/1981 N 1 was officially named Proteus

### Orbital data

Proteus orbits Neptune at ~117,647 km it also has an inclination of about 0.5 degrees and is tidally locked. Proteus might have caused orbital resonance with Larissa several hundred million years ago.
13 Egeria

VLT scan of 13 Egeria

**Egeria** (minor planet designation: **13 Egeria**) is a large main-belt G-type asteroid in the main asteroid belt. It was discovered by Annibale de Gasparis on November 2, 1850. Egeria was named by Urbain Le Verrier, whose computations led to the discovery of Neptune, after the mythological nymph Egeria of Aricia, Italy, the wife of Numa Pompilius, second king of Rome.

Egeria occulted a star on January 8, 1992. Its disc was determined to be quite circular (217×196 km). On January 22, 2008, it occulted another star, and this occultation was timed by several observers in New Mexico and Arizona, coordinated by the IOTA Asteroid Occultation Program. The result showed that Egeria presented an approximately circular profile to Earth of 214.8×192 km, well in agreement with the 1992 occultation. It has also been studied by radar.

In 1988 a search for satellites or dust orbiting this asteroid was performed using the UH88 telescope at the Mauna Kea Observatories, but the effort came up empty. Spectral analysis of Egeria shows it to be unusually high in water content, 10.5–11.5% water by mass. This makes Egeria a prominent candidate for future water-mining ventures.
Rhea

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**Rhea** (/ˈriː.ə/) is the second-largest moon of **Saturn** and the ninth-largest moon in **the Solar System**, with a surface area that is comparable to the area of Australia. It is the smallest body in the Solar System for which precise measurements have confirmed a shape consistent with hydrostatic equilibrium. It was discovered in 1672 by Giovanni Domenico Cassini.

## Rings

Rhea may have a tenuous ring system consisting of three narrow, relatively dense bands within a particulate disk. This would be the first discovery of rings around a moon. The potential discovery was announced in the journal *Science* on March 6, 2008.

In November 2005 the *Cassini* orbiter found that Saturn's magnetosphere is depleted of energetic electrons near Rhea. According to the discovery team, the pattern of depletion is best explained by assuming the electrons are absorbed by solid material in the form of an equatorial disk of particles perhaps several decimeters to approximately a meter in diameter and that contains several denser rings or arcs. Subsequent targeted optical searches of the putative ring plane from several angles by *Cassini'*s narrow-angle camera failed to find any evidence of the expected ring material, and in August 2010 it was announced that Rhea was unlikely to have rings, and that the reason for the depletion pattern, which is unique to Rhea, is unknown. However, an equatorial chain of bluish marks on the Rhean surface suggests past impacts of deorbiting ring material and leaves the question unresolved.
S/2006 S 3

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**S/2006 S 3** is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on June 26, 2006 from observations taken between January and April 2006.

## Physical Characteristics

### Diameter

6 km

S/2006 S 3 is about ~6 kilometres in diameter, and orbits Saturn at an average distance of 21,308,400 km in 1160.7 days, at an inclination of 152.8° to the ecliptic, in a retrograde direction and with an eccentricity of 0.4707.

S/2006 S 3 was considered lost after its discovery and was then recovered in October 2019.
Geirrod

**Geirrod**, provisionally known as **S/2004 S 38**, is a natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, and Jan Kleyna on October 8, 2019 from observations taken between December 12, 2004 and March 22, 2007.

## Designations

### Alternative Names

Saturn LXVI
S/2004 S 38
S8568a

## Physical Characteristics

### Diameter

4 km

It was given its permanent designation **Saturn LXVI** in August 2021 and received its official name 1 year later.

Geirrod is about ~4 kilometres in diameter, and orbits Saturn at an average distance of 21.908 Gm in 1,211.02 days, at an inclination of 154° to the ecliptic, in a retrograde direction and with an eccentricity of 0.437.
Lysithea

Near-infrared 2MASS photograph of Lysithea.

**Lysithea**, formerly known as **Jupiter X**, is an outer irregular satellite of Jupiter that is within the Himalia Group. It’s the 13th largest moon of Jupiter, and 3rd largest in the Himalia Group. Very little is known about Lysithea, primarily due to a lack of interest.

## Discovery

Lysithea was initially discovered when astronomer Seth B. Nicholson found it using the 100-inch telescope at the Mount Wilson Observatory. It was found on July 6, 1938.

## Appearance & Size

It’s not known what Lysithea exactly looks like, as all images of it do not show any details of its surface. However, it’s assumably a small object with a similar appearance to other objects in the Himalia Group. Like other objects in its group, it’s thought that it originated from an asteroid that was torn apart and captured by Jupiter’s gravity or vice versa.

Lysithea has a diameter of about 22.37 miles, making it the 3rd largest object in the Himalia group, and the 13th largest overall.

## Orbit

Similarly to other Himalia Group members, it has a slightly tilted and eccentric orbit. It orbits at 7.2 million miles away from Jupiter, and takes nearly 258.6 days to complete one orbit. This makes it the 15th closest moon to Jupiter.
Ersa

**Ersa**, also designated **Jupiter LXXI**, is a small outer natural satellite of Jupiter discovered by Scott S. Sheppard on 11 May 2018. It was announced along with 9 other moons on 17 July 2018 and it provisionally designated **S/2018 J 1**.

## Ersa

Precovery Image of Ersa taken by Canada-France-Hawaii Telescope in February 2003

## Physical Characteristics

### Diameter

3 km

Ersa belongs to the prograde Himalia group, a collection of prograde natural satellites orbiting the same direction as Jupiter's rotation. Ersa has precovery images dated back on February 24, 2003.
Deimos

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***Deimos*** is the smaller and outermost of the two natural satellites of **Mars**, the other being **Phobos**. Deimos has a mean radius of 6.2 km and takes 30.3 hours to orbit Mars. Deimos is 23,460 km from Mars, much farther than Mars' other moon, Phobos.
15 Eunomia

**Eunomia** (minor planet designation **15 Eunomia**) is a very large asteroid in the middle asteroid belt. It is the largest of the stony (S-type) asteroids, with 3 Juno as a close second. It is quite a massive asteroid, in 6th to 8th place (to within measurement uncertainties). It is the largest Eunomian asteroid, and is estimated to contain 1% of the mass of the asteroid belt.

## Asteroid Data

### Geometric Albedo

0.187

Eunomia was discovered by Annibale de Gasparis on July 29, 1851, and named after Eunomia, one of the Horae (Hours), a personification of order and law in Greek mythology.

## Characteristics

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Titan

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**Titan** is the largest moon of Saturn, the second-largest in the Solar System and larger than any of the dwarf planets of the Solar System. It is the only moon known to have a dense atmosphere, and is the only known object in space other than Earth on which clear evidence of stable bodies of surface liquid has been found.

## Titan

Titan pictured in 2011 in natural color. The thick atmosphere is orange due to a dense organonitrogen haze.

## Designation and Discovery

### Minor Planet Categories

Moons, Saturnian Moons

Titan is one of the seven gravitationally rounded moons in orbit around Saturn, and the second most distant from Saturn of those seven. Frequently described as a planet-like moon, Titan is 50% larger (in diameter) than Earth's Moon and 80% more massive. It is the second-largest moon in the Solar System after Jupiter's moon Ganymede, and is larger than the planet Mercury, but only 40% as massive.

Discovered in 1655 by the Dutch astronomer Christiaan Huygens, Titan was the first known moon of Saturn, and the sixth known planetary satellite (after Earth's moon and the four Galilean moons of Jupiter). Titan orbits Saturn at 20 Saturn radii. From Titan's surface, Saturn subtends an arc of 5.09 degrees, and if it were visible through the moon's thick atmosphere, it would appear 11.4 times larger in the sky, in diameter, than the Moon from Earth, which subtends 0.48° of arc.

Titan is primarily composed of ice and rocky material, which is likely differentiated into a rocky core surrounded by various layers of ice, including a crust of water ice and a subsurface layer of ammonia-rich liquid water. Much as with Venus before the Space Age, the dense opaque atmosphere prevented understanding of Titan's surface until the *Cassini–Huygens* mission in 2004 provided new information, including the discovery of liquid hydrocarbon lakes in Titan's polar regions. The geologically young surface is generally smooth, with few impact craters, although mountains and several possible cryovolcanoes have been found.

The atmosphere of Titan is largely nitrogen; minor components lead to the formation of methane and ethane clouds and heavy organonitrogen haze. The climate—including wind and rain—creates surface features similar to those of Earth, such as dunes, rivers, lakes, seas (probably of liquid methane and ethane), and deltas, and is dominated by seasonal weather patterns as on Earth. With its liquids (both surface and subsurface) and robust nitrogen atmosphere, Titan's methane cycle bears a striking similarity to Earth's water cycle, albeit at the much lower temperature of about 94 K (−179 °C; −290 °F).
19521 Chaos

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**19521 Chaos** is a cubewano, a Kuiper-belt object not in resonance with any planet. Chaos was discovered in 1998 by the Deep Ecliptic Survey with Kitt Peak's 4 m telescope. Its albedo is 0.050+0.030

## 19521 Chaos

19521 Chaos as imaged by the Hubble Space Telescope in September 2001

## Orbit Data

### Aphelion

50.636 AU

−0.016, making it, with its absolute magnitude (H) of 4.8, 600+140

−130 km in diameter.

On 20 November 2020, Chaos occulted a magnitude 16.8 star. Three observers detected the occultation, finding that the object is likely smaller than 600 km in diameter. Another occultation was recorded on 14 January 2022; full results on size, shape, geometric albedo, and the spin-axis orientation have not been released.
2023 FW₁₃

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2023 FW₁₃ is an asteroid that was spotted on March 28, 2023, from the Pan-STARRS telescope at Hawaii, United States. It circles the sun in sync with Earth in such a way that it appears to orbit Earth, but well outside Earth's Hill sphere, making it a quasi-satellite.
J002E3

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This page is incomplete because, **it does not adequately describe its subject**.Please do not remove this tag, unless the page has been completed. You can help the wiki by finishing it.
**This object is/might be not natural**
It may be of artificial origin and may not have formed naturally
**J002E3** is an object in space which is thought to be the S-IVB third stage of the Apollo 12 Saturn V rocket. It was discovered on September 3, 2002, by amateur astronomer Bill Yeung. Initially thought to be an asteroid, it has since been tentatively identified as the third stage of Apollo 12 Saturn V based on spectrographic evidence consistent with the titanium dioxide in the paint used on the rockets. The stage was intended to be injected into a permanent heliocentric orbit in November 1969, but is now believed instead to have gone into an unstable high Earth orbit which left Earth's proximity in 1971 and again in June 2003, with an approximately 40-year cycle between heliocentric and geocentric orbit.
S/2004 S 13

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**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**S/2004 S 13** is a retrograde irregular natural satellite of Saturn. Its discovery was announced by Scott S. Sheppard, David C. Jewitt, Jan Kleyna, and Brian G. Marsden on 4 May 2005 from observations taken between 12 December 2004 and 9 March 2005.

## Physical Characteristics

### Diameter

6 km

S/2004 S 13 is about ~6 kilometres in diameter, and orbits Saturn at an average distance of 18,486,000 kilometres in about 938 days, at an inclination of 167.0° to the ecliptic, in a retrograde direction and with an eccentricity of 0.271.

S/2004 S 13 was considered to be lost after its discovery and was recovered on October 12, 2022.
Kerberos

Featured Article: **This Article Is Recommended For New Users****Kerberos** is a small satellite of the dwarf planet Pluto. It was discovered by the Pluto Companion Search Team when using the Hubble Space Telescope on June 28, 2011.

## Kerberos

Kerberos captured during New Horizon's fly by

## Designations

### Alternative Names

S/2011 (134340) 1
S/2011 P 1

## Orbit Data

### Satellite of

Pluto

moon of Pluto after Styx and measures 19km at it's longest dimension.

## Origin

It has been suspected that Kerberos was formed from an impact that could have likely formed the other moons as well. This theory is similar to the one that created the moon.

## Physical Characteristics

Kerberos appears to be double-lobed in shape, and is approximately 19 km (12 mi) across its longest dimension and 9 km (5.6 mi) across its shortest dimension. It is the second-smallest of Pluto's moons, after Styx. The larger lobe of Kerberos is approximately 8 km (5 mi) across while the smaller lobe is measured to be approximately 5 km (3.1 mi) across. The double-lobed shape of Kerberos is likely formed by two smaller objects merged, suggesting that Kerberos along with Pluto's other moons may have been formed by the coalescence of debris around Pluto.

Kerberos has a very high albedo, consistant with that of ice water.

### Rotation

Like the other moons of Pluto, Kerberos is tidaly locked in place, although it rotates very choaticly, spinning end over end.

## Orbit

Kerberos's orbit is very circular and not inclined. It has an equatorial orbit around the Pluto-Charon barycenter,

with an average distance of 57,783 km. All of Pluto's moons including Kerberos have very circular orbits with very low orbital inclinations to Pluto's equator. Kerberos orbits between Nix and Hydra and makes a complete orbit around Pluto roughly every 32.167 days.

Its orbital period is close to a 1:5 orbital resonance with Charon, with the timing discrepancy being about 0.7%. As with the near resonances between Nix or Hydra and Charon (1:4 and 1:6, respectively), determining how close this relationship is to a true resonance will require more-accurate knowledge of Kerberos's orbit, in particular its rate of precession.
Solarpedia

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Epimetheus

**This page/section has been marked for fixing under Project/Paraphrase**
This page is to be fixed and paraphrased under the project's guidelines. Please do not remove this tag until the project has ended.**Epimetheus** is an inner satellite of Saturn. It is also known as **Saturn XI**. It is named after the mythological Epimetheus, brother of Prometheus.

## Designations

### Categories

Shepherd moon of SaturnCo-orbital with Janus

## Physical Characteristics

### Mean Escape Velocity

0.033 km/s at longest axisto 0.036 km/s at poles

### Albedo (Geometric)

0.73±0.03

Epimetheus occupies essentially the same orbit as the moon Janus. Astronomers assumed that there was only one body in that orbit (disbelieving that two moons could share nearly identical orbits without colliding), and accordingly had difficulty determining their orbital characteristics. Observations were photographic and spaced widely apart in time, so that while the presence of two objects was not obvious, the observations were difficult to reconcile with a reasonable orbit.

## Orbit

Epimetheus's orbit is co-orbital with that of Janus. Janus's mean orbital radius from Saturn is, as of 2006, only 50 km less than that of Epimetheus, a distance smaller than either moon's mean radius. In accordance with Kepler's laws of planetary motion, the closer orbit is completed more quickly.

## Physical Characteristics

Epimetheus has several craters larger than 30 km in diameter, as well as both large and small ridges and grooves. The extensive cratering indicates that Epimetheus must be quite old. Janus and Epimetheus may have formed from a disruption of a single parent to form co-orbital satellites, but if this is the case the disruption must have happened early in the history of the satellite system. From its very low density and relatively high albedo, it seems likely that Epimetheus is a very porous icy body. There is considerable uncertainty in these values, however, and so this remains to be confirmed.

## Interactions with Saturn's Rings

A faint, dusty ring is present around the orbits of Janus and Epimetheus, possibly meaning debris from the moons is forming a thin ring.
Philophrosyne

**Philophrosyne**, also **Jupiter LVIII** and provisionally known as **S/2003 J 15**, is an irregular natural satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard, et al. in 2003

## Physical Characteristics

### Diameter

2 km

Philophrosyne is about ~2 kilometres in diameter, and orbits Jupiter at an average distance of 22,721,000 km in 699.676 days, at an inclination of 142° to the ecliptic, in a retrograde direction and with an eccentricity of 0.0932.

Philophrosyne was considered lost after its discovery and was then recovered in 2017. Along then, it also received its permanent designation.

Philophrosyne belongs to the Pasiphae group, retrograde irregular moons that orbit Jupiter in the opposite direction.
Pandora

**Pandora** is an inner satellite of Saturn. It was discovered in 1980 by *Voyager 1* and was provisionally designated as **S/1980 S 26**. It was given its permanent designation as **Saturn XVII**.

## Discovery

### Discovered by

Stewart A. Collins
D. Carlson
*Voyager 1*

## Physical Characteristics

### Synodic Rotation Period

synchronous

Pandora was thought to be a shepherd moon, until it has been observed that it does not affect the Saturn's F ring. Only Prometheus had an affect on the F ring.
9P/Tempel

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**Tempel 1** or 9P is a periodic Jupiter-family comet discovered by Wilhelm Tempel in 1867. It completes an orbit of the Sun every 5.6 years. Tempel 1 was the target of the Deep Impact space mission, which photographed a deliberate high-speed impact upon the comet in 2005
951 Gaspra

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**951 Gaspra** is an S-type asteroid that orbits very close to the inner edge of the asteroid belt. Gaspra was discovered by Russian astronomer G. N. Neujmin in 1916. Neujmin named it after Gaspra, a Black Sea retreat that was visited by his contemporaries, such as Gorky and Tolstoy.

## 951 Gaspra

Image of Gaspra taken by Galileo in October 29, 1991

## Physical Characteristics

### Mean Density

~2.7 g/cm³

Gaspra was the first asteroid ever to be closely approached when it was visited by the *Galileo* spacecraft, which flew by on its way to Jupiter on 29 October 1991.
Mundilfari

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**Mundilfari**, or **Saturn XXV**, is a retrograde irregular natural satellite of Saturn. It was discovered by Brett J. Gladman, et al. in 2000, and given its provisional designation **S/2000 S 9**.

## Mundilfari

Images of Mundilfari taken by Canada-France-Hawaii Telescope in September 2000

## Physical Characteristics

### Synodic Rotation Period

6.74 h

Mundilfari is about ~7km in diameter and could potentially be a fragment piece of Phoebe.