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Eris (dwarf planet)

Eris also designated (136199) Eris or 136199 Eris, is the largest known dwarf planet in the solar system and the ninth largest body orbiting the Sun. It is a trans-Neptunian object (TNO), orbiting the Sun in a region of space known as the scattered disc, just beyond the Kuiper belt, and accompanied by at least one moon, Dysnomia. Mike Brown, who led the Mount Palomar-based discovery team, announced in April 2006 that the Hubble Telescope has measured Eris's diameter to be 2400 km, slightly larger than that of Pluto.[4]

Eris' size resulted in its discoverers and NASA labelling it the solar system's tenth planet. This, along with the prospect of other similarly sized objects being discovered in the future, stimulated the International Astronomical Union (IAU) to define the term "planet" more precisely. Under a new definition approved on August 24, 2006, Eris was designated a "dwarf planet" along with Pluto and Ceres.[5] Brown has since stated his approval of the new "dwarf planet" label.[6]


Eris was discovered by the team of Mike Brown, Chad Trujillo, and David Rabinowitz on January 5, 2005, from images taken on October 21, 2003. The discovery was announced on July 29, 2005, the same day as two other large TNOs, (136108) 2003 EL61 and (136472) 2005 FY9. The search team has been systematically scanning for large outer solar system bodies for several years, and had previously been involved in the discovery of several other very large TNOs, including 50000 Quaoar, 90482 Orcus, and 90377 Sedna.

Routine observations were taken by the team on October 21, 2003, using the 48-inch (122 cm) Samuel Oschin reflecting telescope at Mount Palomar Observatory, California, but the object captured on the images was not discovered at that point due to its very slow motion across the sky: the team's automatic image-searching software excluded all objects moving at less than 1.5 arcseconds per hour to reduce the number of false positives returned. When Sedna was discovered, it was moving at 1.75 arcsec/h, and in light of that the team reanalyzed their old data with a lower limit on the angular motion, sorting through the previously excluded images by eye. In January 2005, the re-analysis revealed Eris' slow motion against the background stars.

Follow-up observations were then carried out to make a preliminary determination of its orbit, which allowed its distance and size to be estimated. The team had planned to delay announcing their discovery until further observations had been made which would have allowed more accurate determinations of the body's size and mass, but were forced to bring forward the announcement when the discovery of another object they had been tracking (2003 EL61) was announced by another group in Spain.

Yet more observations released in October 2005 revealed that the object had a moon, later named Dysnomia. Scientists plan to use this information to determine the mass of Eris.

Discovered by: M. E. Brown,
C. A. Trujillo,
D. L. Rabinowitz[1]
Discovery date: October 21, 2003[1]
MPC designation: 136199 Eris
Alternative names: 2003 UB313 [2]
Minor planet category: dwarf planet
TNO (scattered disc object)
Orbital characteristics
Epoch March 6, 2006
(JD 2453800.5) [3]
Aphelion distance: 97.56 AU (14.60 Tm)
Perihelion distance: 37.77 AU (5.65 Tm)
Semi-major axis: 67.6681 AU (10.12 Tm)
Eccentricity: 0.44177
Sidereal period: 203,500 d (557 a)
Avg. orbital speed: 3.436 km/s
Max. orbital speed: 4.126 km/s
Min. orbital speed: 2.567 km/s
Mean anomaly: 197.63427°
Inclination: 44.187°
Longitude of ascending node: 35.8696°
Argument of perihelion: 151.4305°
Physical characteristics
Equatorial radius: 1200 km ± 50 km
(750 mi ± 30 mi,
or 19% of Earth)
Sidereal rotation period: > 8 h?
Albedo: 0.86 ± 0.07
Surface temp.:
min mean max
  ~30 K  
Absolute magnitude: −1.12 ± 0.01


Eris is classified as a dwarf planet and a scattered disk object (SDO).[7] The latter is a category of the TNOs that are believed to have been "scattered" from the Kuiper belt into more distant and unusual orbits following gravitational interactions with Neptune as the solar system was forming. Although its high orbital inclination is unusual among the known SDOs, theoretical models suggest that objects that were originally near the inner edge of the Kuiper belt are scattered into orbits with higher inclinations than objects from the outer belt. Inner-belt objects are expected to be generally more massive than outer-belt objects, and so astronomers expect to discover more large objects like Eris in high-inclination orbits.

As Eris is larger than Pluto, it was initially described as the "tenth planet" by NASA and in media reports of its discovery. In response to the uncertainty over its status, and because of continuing debate over whether Pluto should be classified as a planet, the IAU delegated a group of astronomers to develop a new definition of the term planet. This definition was clarified under the new IAU definition of a planet, adopted on 24 August 2006. Eris has been termed a dwarf planet by the IAU. It may also be under consideration as a member of "a new class of trans-Neptunian objects" yet to be defined by that body. It is not, however, considered to be a planet.


Eris is named after the goddess Eris (Greek Ἔρις), a personification of strife and discord.[8] This name was assigned on September 13, 2006 following an unusually long period in which it was best known by the provisional designation 2003 UB313, which was granted automatically by the IAU under their naming protocols for minor planets.


Before the name Eris was granted, two nicknames were used for the planet by the popular media.

  • "Xena" was an informal name used by the discovery team. It was inspired by eponymous heroine of the television series Xena: Warrior Princess. The discovery team had reportedly saved the nickname 'Xena' for the first body they discovered that was larger than Pluto. Their only stated reason was that "We have always wanted to name something Xena"[9] (apparently implying that the name was chosen without any reference to Planet X).
  • The nickname "Lila" has also been used, but this is a misunderstanding of planetlila, part of the URL of the discovery web page;[10] the web page's name was derived from the name of Mike Brown's then-newborn daughter, Lilah.

Choosing an official name

The delay in assigning a name was due to uncertainty over whether the object was classified as a planet or a minor planet; different nomenclature procedures apply to these different classes of object. [11] The decision on a name had to wait until after the August 24, 2006 IAU ruling defining the object as a dwarf planet.[12]

Brown had previously speculated that Persephone would be a good name for the object. However, this was not possible once the object was classified as a dwarf planet, because there is already an asteroid with that name (399 Persephone).[13] Since IAU regulations demand a name from a creation mythology for objects with orbital stability beyond Neptune's orbit, the team had also been considering such possibilities.[10]

The discovery team proposed 'Eris' on 6 September 2006, and on 13 September 2006, it was accepted as the official name by the IAU.[14][10] The name in part reflects the discord in the astronomical community caused by the debate over the object's nature.

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Eris has an orbital period of 556.7 years, and currently lies at almost its maximum possible distance from the Sun (aphelion). It is currently the most distant known solar system object from the Sun at a distance of roughly 97 astronomical units. Its semimajor axis is 67.669 AU, its perihelion distance is 37.78 AU, and its aphelion distance is 97.56 AU. Approximately forty known TNOs (most notably 2000 OO67 and Sedna), while currently closer to the Sun than Eris, have greater average orbital distances.[15]

Its orbit is highly eccentric, and brings it to within 37.8 AU of the Sun (a typical perihelion for scattered objects), still safe from direct interaction with Neptune (at ~30 AU). For comparison, Pluto, like other plutinos, follows a less inclined and less eccentric orbit and, protected by orbital resonance, it can cross Neptune’s orbit. Unlike the terrestrial planets and gas giants, whose orbits all lie roughly in the same plane as the Earth's, Eris' orbit is very inclined — it is tilted at an angle of about 44 degrees to the ecliptic.

The object currently has an apparent magnitude of about 19, making it bright enough to be detectable in some amateur telescopes. A telescope with an 8" lens or mirror and a CCD can detect Eris under favorable conditions.[16] The reason it had not been noticed until now is because of its steep orbital inclination: most searches for large outer solar system objects concentrate on the ecliptic plane, in which most solar system material is found.

Eris is now in the constellation Cetus. It was in Sculptor until 1929, and will enter Pisces in 2036.[17] Because the orbit of Eris is highly inclined, it only passes through a few constellations of the traditional Zodiac.


Optical measurement from HST pictures

The diameter of Eris has been measured to be 2400 km using images from the Hubble Space Telescope. The brightness of an object depends both on its size and the amount of light it reflects (its albedo). At a distance of 67 AU, an object with a radius of 3000 km would have an angular size of 40 milliarcseconds, which is directly measurable with HST; although resolving such small objects is at the very limit of Hubble's capabilities,[18] sophisticated image processing techniques such as deconvolution can be used to measure such angular sizes fairly accurately.[19]

This revised estimate of the diameter makes Eris only 4% larger than Pluto According to Hubble, Eris' diameter measures 2,397 km (1,490 mi), give or take 100 km (60 mi). Pluto is about 2,306 km (1,433 mi) across. It also indicates that the albedo is 0.86, higher than any other large body in the solar system other than Enceladus. It is speculated that the high albedo is due to the surface ices being replenished due to temperature fluctuations as Eris' eccentric orbit takes it closer and farther from the Sun.

Thermal measurement

Previous observations of the thermal emission of Eris at a wavelength of 1.2 mm, where the object's brightness depends only on temperature and surface area, indicated a diameter of 3000 km, about a third larger than Pluto. If the object rotates quickly, resulting in a more even heat distribution and a temperature of 23 to 24 kelvins, a likely diameter would be in the higher portion of the range (best fit 3090 km); if it rotates slowly, the visible surface would be warmer (about 27 K) and a likely diameter would be in the smaller end of the range (best fit 2860 km). The 2860 km figure implies a Pluto-like albedo of 60%, consistent with its Pluto-like spectral signature.

Possible explanation of the inconsistent results

The apparent inconsistency of the HST PSF results (2400 ± 100 km) with the above IRAM results (3000 ± 370 km) will certainly be studied at more length. Brown explains it by a slightly lower absolute magnitude than the one assumed by Bertoldi (−1.12 ± 0.01 versus −1.16 ± 0.1, resulting by itself in almost 100 km difference in diameter). Assuming further the highest diameter (2500 km) and pole-on position of the object[21] the difference between the results would appear consistent with 1.1-σ error margin.

Another possible explanation for the IRAM results is offered by the Max-Planck-Institut für Radioastronomie. The ratio between the bolometric albedo (representing the total reflected energy and used in the thermal method) and the geometric albedo (representing the reflection in some visual wavelength and used to calculate the diameter from HST pictures) is not known with high precision and depends on many factors. By itself, this uncertainty could bridge the gap between the two measures.[20]


The discovery team followed up their initial identification of Eris with spectroscopic observations made at the 8 m Gemini North Telescope in Hawaii on January 25, 2005. Infrared light from the object revealed the presence of methane ice, indicating that the surface of Eris is rather similar to Pluto, which was the only TNO already known to show the presence of methane. Neptune's moon Triton is probably related to Kuiper Belt objects, and also has methane on its surface.

Unlike the somewhat reddish Pluto and Triton, however, Eris appears almost grey. Pluto's reddish color is believed to be due to deposits of tholins on its surface, and where these deposits darken the surface, the lower albedo leads to higher temperatures and the evaporation of methane deposits. In contrast, Eris is far enough away from the Sun that methane can condense onto its surface even where the albedo is low. The condensation of methane uniformly over the surface reduces any albedo contrasts and would cover up any deposits of red tholins.

Methane is very volatile and its presence shows either that Eris has always resided in the distant reaches of the solar system where it is cold enough for methane ice to persist, or that it has an internal source of methane to replenish gas that escapes from its atmosphere. This contrasts with observations of another recently-discovered TNO, 2003 EL61, which reveal the presence of water ice but not methane.


Even though Eris can be up to three times further from the Sun than Pluto, it approaches close enough that some of the various ices that exist on the surface might become warm enough to sublimate and form a fine atmosphere; however, it is unclear whether this actually happens on Eris.

Due to its orbit, surface temperatures vary between about −232 and −248 degrees Celsius.


During 2005, the adaptive optics team at the Keck telescopes in Hawaii carried out observations of the four brightest TNOs (Pluto, 2005 FY9, 2003 EL61, and Eris), using the newly commissioned laser guide star adaptive optics system. Observations taken on September 10 revealed a moon in orbit around Eris, which received its name (Dysnomia) at the same time as its primary. In keeping with the "Xena" nickname already in use for Eris, the moon was previously nicknamed Gabrielle by its discoverers, after the television warrior princess's sidekick. The name Dysnomia is taken from a mythological demon of lawlessness who was Eris' daughter. Brown's group has pointed out the link with the former nicknames, as the character of Xena was played by Lucy Lawless.[10]

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