Eris
|
Discovery |
Discovered by |
|
Discovery date |
January 5, 2005[2][a] |
Designations |
MPC designation |
136199 Eris |
Pronunciation |
or [b] |
Named after
|
Eris |
|
2003 UB313[3] |
|
|
Adjectives |
Eridian |
Orbital characteristics[3] |
Epoch 2014-Dec-09
(JD 7006245700050000000♠2457000.5) |
Aphelion |
- 7013146083816717260♠97.651 AU
- 7013146020000000000♠14.602×109 km
|
Perihelion |
- 7012567140487610770♠37.911 AU
- 7012572300000000000♠5.723×109 km
|
|
- 7013101398932739170♠67.781 AU
- 7013101660000000000♠10.166×109 km
|
Eccentricity |
6999440680000000000♠0.44068 |
|
- 7010176109120000000♠203830 d
- 7002558040000099999♠558.04 years
|
|
7003343380000000000♠3.4338 km/s |
|
7000356326420087160♠204.16° |
Inclination |
6999768721542394640♠44.0445° |
|
6999627499971298770♠35.9531° |
|
7000263504574478350♠150.977° |
Known satellites |
Dysnomia |
Physical characteristics |
Mean radius
|
7006116300000000000♠1163±6 km[8][9] |
|
7013170000000000000♠17000000 km2 |
Mass |
|
|
7003252000000000000♠2.52±0.05 g/cm3[8][11] |
|
0.793 m/s2
0.084 g[12] |
|
1.384 km/s |
|
7001259000000000000♠25.9±8 hr[3] |
Albedo |
6999960000000000000♠0.96+0.09
−0.04[8] |
Surface temp. |
min |
mean |
max |
(approx) |
30 K |
42.5 K |
55 K |
|
Spectral type
|
B−V=0.78, V−R=0.45[13] |
|
18.7[14] |
|
2999880000000000000♠−1.2±0.3[3] |
|
40 milli-arcsec[15] |
Eris (
minor-planet designation 136199 Eris) is the most massive
dwarf planet known in the
Solar System, and the ninth most massive body known to directly orbit the
Sun. It was measured to be 2,326 ± 12 kilometers (1,445.3 ± 7.5 mi) in diameter.
[8] Eris is 27% more
massive than dwarf planet
Pluto, though Pluto is slightly larger by volume. Eris' mass is about 0.27% of the
Earth's mass.
[10][16]
Eris was discovered in January 2005 by a
Palomar Observatory–based team led by
Mike Brown, and its identity was verified later that year. It is a
trans-Neptunian object (TNO) and a member of a high-eccentricity population known as the
scattered disk. It has one known
moon,
Dysnomia. As of 2014
[update], its distance from the Sun is 96.4 astronomical units (1.442
×10
10 km; 8.96
×10
9 mi),
[14] roughly three times that of Pluto. With the exception of some
comets, Eris and Dysnomia are currently the most distant known natural objects in the Solar System.
[2][d]
Because Eris appeared to be larger than Pluto,
NASA initially described it as the Solar System's
tenth planet. This, along with the prospect of other objects of similar size being discovered in the future, motivated the
International Astronomical Union (IAU) to
define the term planet for the first time. Under the
IAU definition approved on August 24, 2006, Eris is a "dwarf planet", along with objects such as Pluto,
Ceres,
Haumea and
Makemake,
[19] thereby reducing the number of known planets in the Solar System to eight, the same number as before Pluto's discovery in 1930. Observations of a stellar
occultation by Eris in 2010 showed that its diameter was 2,326 ± 12 kilometers (1,445.3 ± 7.5 mi), not significantly different from that of Pluto.
[20][21] After
New Horizons measured Pluto's diameter as 2370 km in July 2015, it was proven that Eris is slightly smaller in diameter than Pluto.
[22]
Discovery
Eris was discovered by the team of
Mike Brown,
Chad Trujillo, and
David Rabinowitz[2] on January 5, 2005, from images taken on October 21, 2003. The discovery was announced on July 29, 2005, the same day as
Makemake and two days after
Haumea,
[23] due in part to
events that would later lead to controversy about Haumea. The search team had been systematically scanning for large outer
Solar System bodies for several years, and had been involved in the discovery of several other large TNOs, including
50000 Quaoar,
90482 Orcus, and
90377 Sedna.
Routine observations were taken by the team on October 21, 2003, using the 1.2 m
Samuel Oschin Schmidt telescope at
Palomar Observatory, California, but the image of Eris 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's slow motion against the background
stars.
Animation showing the movement of Eris on the images used to discover it. Eris is indicated by the arrow. The three frames were taken over a period of three hours.
Distribution of trans-Neptunian objects
Follow-up observations were then carried out to make a preliminary determination of Eris's
orbit, which allowed the object's distance to be estimated. The team had planned to delay announcing their discoveries of the bright objects Eris and
Makemake until further observations and calculations were complete, but announced them both on July 29 when the discovery of another large TNO they had been tracking,
Haumea, was
controversially announced on July 27 by a different team in Spain.
[2]
More observations released in October 2005 revealed that Eris has a moon, later named
Dysnomia. Observations of Dysnomia's orbit permitted scientists to determine the mass of Eris, which in June 2007 they calculated to be
7022167000000000000♠(1.67±0.02)×1022 kg,
[10] 27% greater than Pluto's.
Classification
Eris is a
trans-Neptunian dwarf planet (
plutoid).
[24] Its orbital characteristics more specifically categorize it as a
scattered-disk object (SDO), or a TNO that is 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 were scattered into orbits with higher inclinations than objects from the outer belt.
[25] 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, which have traditionally been neglected.
Because Eris was initially believed to be larger than
Pluto, it was described as the "
tenth planet" by
NASA and in media reports of its discovery.
[26] In response to the uncertainty over its status, and because of ongoing debate over whether Pluto should be classified as a
planet, the IAU delegated a group of astronomers to develop a sufficiently precise definition of the term
planet to decide the issue. This was announced as the IAU's
Definition of a Planet in the Solar System, adopted on August 24, 2006. At this time, both Eris and Pluto were classified as
dwarf planets, a category distinct from the new definition of
planet.[27] Brown has since stated his approval of this classification.
[28] The IAU subsequently added Eris to its
Minor Planet Catalogue, designating it
(136199) Eris.[29]
Name
Eris is named after the goddess
Eris (Greek
Ἔρις), a personification of strife and discord.
[30] The name was assigned on September 13, 2006, following an unusually long period in which the object was known by the
provisional designation 2003 UB313, which was granted automatically by the IAU under their naming protocols for
minor planets. The regular adjectival form of
Eris is
Eridian.
Xena
Due to uncertainty over whether the object would be classified as a
planet or a
minor planet, because different nomenclature procedures apply to these different classes of objects,
[31] the decision on what to name the object had to wait until after the August 24, 2006, IAU ruling.
[29] As a result, for a time the object became known to the wider public as
Xena.
"Xena" was an informal name used internally by the discovery team. It was inspired by the title character 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. According to Brown,
We chose it since it started with an X (planet "X"), it sounds mythological (OK, so it's TV mythology, but Pluto is named after a cartoon, right?),[e] and (this part is actually true) we've been working to get more female deities out there (i.e. Sedna). Also, at the time, the TV show was still on TV, which shows you how long we've been searching![33]
"We assumed [that] a real name would come out fairly quickly, [but] the process got stalled," Mike Brown said in interview,
One reporter called me up from the New York Times who happened to have been a friend of mine from college, [and] I was a little less guarded with him than I am with the normal press. He asked me, "What's the name you guys proposed?" and I said, "Well, I'm not going to tell." And he said, "Well, what do you guys call it when you're just talking amongst yourselves?"... As far as I remember this was the only time I told anybody this in the press, and then it got everywhere, which I only sorta felt bad about—I kinda like the name.[34]
Choosing an official name
Artist's impression of the dwarf planet Eris. This artistic representation is based on observations made at
ESO's
La Silla Observatory.
[35]
According to science writer
Govert Schilling, Brown initially wanted to call the object "
Lila", after a concept in
Hindu mythology that described the cosmos as the outcome of a game played by
Brahma. The name was very similar to "Lilah", the name of Brown's newborn daughter. Brown was mindful of not making his name public before it had been officially accepted. He had done so with
Sedna a year previously, and had been heavily criticized. He listed the address of his personal web page announcing the discovery as
/~mbrown/planetlila and in the chaos following the
controversy over the discovery of Haumea, forgot to change it. Rather than needlessly anger more of his fellow astronomers, he simply said that the webpage had been named for his daughter and dropped "Lila" from consideration.
[36]
Brown had also speculated that
Persephone, the wife of the god
Pluto, would be a good name for the object.
[2] The name had been used several times in
science fiction,
[37] and was popular with the public, having handily won a poll conducted by
New Scientist magazine ("Xena", despite only being a nickname, came fourth).
[38] This was not possible once the object was classified as a dwarf planet, because there is already an
asteroid with that name,
399 Persephone.
[2]
With the dispute resolved, the discovery team proposed
Eris on September 6, 2006. On September 13, 2006 this name was accepted as the official name by the IAU.
[39][40] Brown decided that, because the object had been considered a
planet for so long, it deserved a name from
Greek or
Roman mythology, like the other planets. The asteroids had taken the vast majority of Graeco-Roman names.
Eris, whom Brown described as his favorite goddess, had fortunately escaped inclusion.
[34] The name in part reflects the discord in the astronomical community caused by the debate over the object's (and Pluto's) nature.
Orbit
The orbit of Eris (blue) compared to those of
Saturn,
Uranus, Neptune, and Pluto (white/gray). The arcs below the ecliptic are plotted in darker colors, and the red dot is the Sun. The diagram on the left is a polar view whereas the diagrams on the right are different views from the ecliptic.
The distances of Eris and Pluto from the Sun in the next 1,000 years
Eris has an
orbital period of 558
years.
[14] Its maximum possible distance from the
Sun (
aphelion) is 97.65
AU, and its closest (perihelion) is 37.91 AU.
[14] It came to
perihelion between 1698
[5] and 1699,
[41] to aphelion around 1977,
[41] and will return to perihelion around 2256
[41] to 2258.
[42] Eris and its moon are currently the most distant known objects in the Solar System apart from
long-period comets and
space probes.
[43] Approximately forty known
TNOs, most notably
2006 SQ372,
2000 OO67 and
Sedna, though currently closer to the Sun than Eris, have greater average orbital distances than Eris's
semimajor axis of 67.7 AU.
[4]
Eris's orbit is highly
eccentric, and brings Eris to within 37.9 AU of the Sun, a typical perihelion for
scattered objects. This is within the orbit of Pluto, but still safe from direct interaction with Neptune (29.8–30.4 AU). Pluto, on the other hand, like other
plutinos, follows a less inclined and less eccentric orbit and, protected by
orbital resonance, can cross Neptune's orbit. It is possible that Eris is in a 17:5 resonance with Neptune, though further observations will be required to check that hypothesis.
[44] Unlike the eight planets, whose orbits all lie roughly in the same plane as the Earth's, Eris's orbit is highly
inclined: It is tilted at an angle of about 44
degrees to the
ecliptic. In about 800 years, Eris will be closer to the Sun than Pluto for some time (see the graph at the right).
Eris currently has an
apparent magnitude of 18.7, making it bright enough to be detectable to some amateur
telescopes. A 200 millimetres (7.9 in) telescope with a
CCD can detect Eris under favorable conditions.
[f] The reason it had not been noticed until now is its steep orbital inclination; most searches for large outer Solar System objects concentrate on the ecliptic plane, where most bodies are found.
Because of the high inclination of its orbit, Eris only passes through a few constellations of the traditional
Zodiac; it is now in the constellation
Cetus. It was in
Sculptor from 1876 until 1929 and
Phoenix from roughly 1840 until 1875. In 2036 it will enter
Pisces and stay there until 2065, when it will enter
Aries.
[41] It will then move into the
northern sky, entering
Perseus in 2128 and
Camelopardalis (where it will reach its northernmost
declination) in 2173.
Size, mass and density
In 2005, the
diameter of Eris was measured to be
7006239700000000000♠2397±100 km, using images from the
Hubble Space Telescope (HST).
[45][47] The size of an object is determined from its
absolute magnitude (H) and the
albedo (the amount of light it reflects). At a distance of 97 AU, an object with a diameter of 3,000 km would have an
angular size of 40
milliarcseconds,
[15] which is directly measurable with the Hubble Space Telescope. Although resolving such small objects is at the very limit of the telescope's capabilities,
[g] sophisticated image processing techniques such as
deconvolution can be used to measure such angular sizes fairly accurately.
[h]
This makes Eris around the same size as Pluto, which is
7006237000000000000♠2370 km across. It also indicates an
albedo of 0.96, higher than that of any other large body in the Solar System except
Enceladus.
[8] It is speculated that the high albedo is due to the surface ices being replenished because of temperature fluctuations as Eris's eccentric orbit takes it closer and farther from the Sun.
[49]
In 2007, a series of observations of the largest trans-Neptunian objects with the
Spitzer Space Telescope gave an estimate of Eris's diameter of
7006260000000000000♠2600+400
−200 km.
[46] The Spitzer and Hubble estimates overlap in the range of 2,400–2,500 km, 4–8% larger than Pluto. Astronomers now suspect that Eris's spin axis is currently pointing toward the Sun, which would make the sunlit hemisphere warmer than average and skew any
infrared measurements toward higher values.
[9] So the outcome from the 2010 Chile
occultation is actually more in line with the Hubble result from 2005.
[9]
In November 2010, Eris was the subject of one of the most distant stellar occultations yet from Earth.
[9] Preliminary data from this event cast doubt on previous size estimates.
[9] The teams announced their final results from the occultation in October 2011, with an estimated diameter of
7006232600000000000♠2326+6
−6 km.
[8] The mass of Eris can be calculated with much greater precision. Based on the currently accepted value for Dysnomia's period—15.774 days—
[10][50] Eris is 27 percent more massive than Pluto. If the 2011 occultation results are used, then Eris has a density of
7003252000000000000♠2.52±0.05 g/cm3, substantially denser than Pluto, and thus must be composed largely of rocky materials.
[8]
Models of internal heating via
radioactive decay suggest that Eris could have an
internal ocean of liquid water at the mantle–core boundary.
[51]
In July of 2015, after nearly ten years of being considered the ninth-largest object known to directly orbit the sun, close-up imagery from the
New Horizons mission more accurately determined
Pluto's volume to be slightly larger than Eris's, rather than slightly smaller as previously thought. Eris is now the tenth-largest object known to directly orbit the sun by volume, though not by mass.
[52]
Surface and atmosphere
The infrared spectrum of Eris, compared to that of Pluto, shows the marked similarities between the two bodies. Arrows denote methane absorption lines.
Artist's impression of Eris and Dysnomia. Eris is the main object, Dysnomia the small gray sphere just above it. The flaring object top-left is the Sun.
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 may be similar to that of Pluto, which at the time was the only
TNO known to have surface methane, and of Neptune's moon
Triton, which also has methane on its surface.
[53] No surface details can be resolved from Earth or its orbit with any instrument currently available.
Due to Eris's distant eccentric orbit, its surface temperature is estimated to vary between about 30 and 56 K (−243.2 and −217.2 °C).
[2]
Unlike the somewhat reddish Pluto and Triton, Eris appears almost white.
[2] 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 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.
[54]
Even though Eris can be up to three times farther from the Sun than Pluto, it approaches close enough that some of the ices on the surface might warm enough to
sublime. Because methane is highly
volatile, 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 the celestial body has an internal source of methane to replenish gas that escapes from its
atmosphere. This contrasts with observations of another discovered TNO,
Haumea, which reveal the presence of
water ice but not methane.
[55]
Moon
In 2005, the
adaptive optics team at the
Keck telescopes in Hawaii carried out observations of the four brightest
TNOs (Pluto,
Makemake,
Haumea, and Eris), using the newly commissioned
laser guide star adaptive optics system.
[56] Images taken on September 10 revealed a
moon in orbit around Eris. In keeping with the "Xena" nickname already in use for Eris, Brown's team nicknamed the moon "
Gabrielle", after the television warrior princess' sidekick. When Eris received its official name from the IAU, the moon received the name
Dysnomia, after the
Greek goddess of lawlessness who was Eris's daughter. Brown says he picked it for similarity to his wife's name, Diane. The name also retains an oblique reference to Eris's old informal name
Xena, portrayed on TV by
Lucy Lawless.
[57]