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90482 Orcus

90482 Orcus
Discovered by M. Brown,
C. Trujillo,
D. Rabinowitz
Discovery date February 17, 2004
MPC designation 90482 Orcus
Named after
2004 DW
possible plutoid
Adjectives Orcean
Orbital characteristics[1]
Epoch July 23, 2010 (JD 2455400.5)
Aphelion 48.07 AU (7.19117 Tm)
Perihelion 30.27 AU (4.52833 Tm)
39.173 AU (5.86018 Tm)
Eccentricity 0.22718
245.18 yr (89552 d)
Inclination 20.573°
Known satellites Vanth (276±17 km, assuming equal albedo)
Physical characteristics
Dimensions 917±25 km[4]
Mass (6.41±0.19)×1020 kg (system)[5]
Mean density
≈ 0.18 m/s2
≈ 0.41 km/s
13.188 hr[6]
Albedo 0.231+0.018
Temperature < 44 K[6]
Spectral type
B−V=0.68; V−R=0.37[7]
19.1 (opposition)[8][9]
2.31±0.03 (integral)[4]
primary: 2.41±0.05[10]
satellite: 4.88±0.05[10]

90482 Orcus is a Kuiper belt object with a large moon, Vanth. It was discovered on February 17, 2004 by Michael Brown of Caltech, Chad Trujillo of the Gemini Observatory, and David Rabinowitz of Yale University. Precovery images as early as November 8, 1951 were later identified.[1] It is probably a dwarf planet.

Orcus is a plutino, locked in a 2:3 resonance with Neptune, making two revolutions around the Sun to every three of Neptune's. This is much like Pluto, except that it is constrained to always be in the opposite phase of its orbit from Pluto: Orcus is at aphelion when Pluto is at perihelion and vice versa. Moreover, the aphelion of Orcus's orbit points in nearly the opposite direction from Pluto's, although the eccentricities and inclinations are similar. Because of these similarities and contrasts, along with its large moon Vanth that recalls Pluto's large moon Charon, Orcus has been regarded as the anti-Pluto. This was a major consideration in selecting its name, as the deity Orcus was the Etruscan equivalent of the Roman Pluto, and later became an alternate name for Pluto.[11]

The surface of Orcus is relatively bright with albedo reaching 30%, grey in color and water-rich. The ice is predominantly in crystalline form, which may be related to past cryovolcanic activity. Other compounds like methane or ammonia may also be present. The existence of a satellite allowed astronomers to determine the mass of the system, which is approximately equal to that of the Saturnian moon Tethys. The ratio of masses of Orcus and Vanth is uncertain, possibly anywhere from 1:33 to 1:12. The diameter of Orcus is estimated to be 761 or 807 km and the diameter of Vanth 378 or 267 km respectively, depending on their relative albedos.[5]


  • Orbit and rotation 1
  • Name 2
  • Physical characteristics 3
    • Size and magnitude 3.1
    • Mass and density 3.2
    • Spectra and surface 3.3
    • Comparison with moons and other TNOs 3.4
    • Cryovolcanism 3.5
  • Satellite 4
  • References 5
  • External links 6

Orbit and rotation

The orbits of Orcus (blue), Pluto (red) and Neptune (grey). Orcus and Pluto are shown in the April 2006 positions. The dates of their perihelia (q) and aphelia (Q) are also marked.

Orcus is in 2:3 orbital resonance with Neptune,[2] having an orbital period of 247 years. Orcus's orbit is similar to Pluto's (both have perihelia above the ecliptic), but is oriented differently. Although at one point its orbit approaches that of Neptune, the resonance between the two bodies means that Orcus itself is always a great distance away from Neptune (there is always an angular separation of over 60 degrees between them). Over a 14,000-year period Orcus stays more than 18 AU from Neptune.[12] Because their mutual resonance with Neptune constrains Orcus and Pluto to remain in opposite phases of their otherwise very similar motions, Orcus is sometimes described as the "anti-Pluto".[11]

Orcus is currently 48.0 AU from the Sun[8] and will come to aphelion (farthest distance from the Sun) in 2019.[9] Simulations by the Deep Ecliptic Survey (DES) show that over the next 10 million years Orcus can acquire a perihelion distance (qmin) as small as 27.8 AU.[2]

The rotation period of the primary is not known. Different photometric surveys have produced different results. Some show low amplitude variations with periods ranging from 7 to 21 hours, whereas others show no variability.[13] However, the value obtained by Ortiz et al., about 10.5 hours, seems to be the most likely one.[14] The rotational poles of Orcus probably coincide with the orbital poles of its moon, Vanth. This means that Orcus is currently viewed pole-on, which could explain the near absence of any rotational modulation of its brightness.[13][14] If, however, the primary is tidally locked with the satellite, the rotational period will coincide with the 9.7-day orbital period of Vanth.[14]


(90482) 2004 DW was assigned the name Orcus on November 22, 2004.[15]

Under the guidelines of the International Astronomical Union's naming conventions, objects with a similar size and orbit to that of Pluto are named after underworld deities. Accordingly, the discoverers suggested naming the object after Orcus, the Etruscan god of the underworld and punisher of broken oaths. He was portrayed in paintings in Etruscan tombs as a hairy, bearded giant. The name was also a private reference to the homonymous Orcas Island, where Brown's wife Diane had lived as a child and that they visit frequently.[16]

On March 30, 2005, Orcus's companion, Vanth was named after a winged female demon of the Etruscan underworld. She could be present at the moment of death, and frequently acted as a guide of the deceased to the underworld.[15]

Physical characteristics

Size and magnitude

The absolute magnitude of Orcus is approximately 2.3[4] (comparable with the 2.6 of cubewano 50000 Quaoar). The detection of Orcus by the Spitzer Space Telescope in the far infrared[17] and by Herschel Space Telescope in submillimeter constrains its diameter to 958.4±22.9 km.[4] Orcus appears to have an albedo of about 21% to 25%,[4] which may be typical of trans-Neptunian objects approaching the 1000 km diameter range.[18]

In the magnitude and size estimates reported above it was assumed that Orcus is a singular object. The presence of a relatively large satellite (Vanth, see below) may change them considerably. The absolute magnitude of Vanth is estimated at 4.88, which means that it is about 11 times fainter than Orcus itself.[10] If the albedos of both bodies are the same at 0.23 then the size of Orcus is about 917±25 km, and the size of Vanth is about 276±17 km.[4]

Orcus compared to Earth and the Moon

Mike Brown's website lists Orcus as a dwarf planet with "near certainty",[19] Tancredi concludes that it is one,[20] and is massive enough to be considered one under the 2006 draft proposal of the IAU,[21] but the IAU has not formally recognized it as such.[22][23]

Mass and density

Since Orcus is known to be a binary system, the mass of the system has been estimated to be (6.32±0.05)×1020 kg, or about 3.8% the mass of the most massive known dwarf planet, Eris.[10] How this mass is partitioned between Orcus and Vanth depends of their relative sizes. If Vanth's diameter is about one third that of Orcus, its mass is only 3% of the system mass. On the other hand, if the size of Vanth is about half that of the primary (see above), then its mass could be as high as 1/12 of the system mass, or about 8% of the mass of Orcus.[10]

The density of the primary (and secondary assuming the same density) is about 1.5 g/cm3.[4]

Spectra and surface

The orbital resonances of Orcus and Pluto in a rotating frame with a period equal to Neptune's orbital period. (Neptune is held stationary.)

The first spectroscopic observations in 2004 showed that the visible spectrum of Orcus is flat (neutral in color) and featureless, whereas in the near-infrared there were moderately strong water absorption bands at 1.5 and 2.0 μm. Thus Orcus appeared to be different from other trans-Neptunian objects like Ixion with red visible and often featureless infrared spectra.[24] Further Infrared observations in 2004 by the European Southern Observatory and the Gemini telescope give results consistent with mixtures of water ice and carbonaceous compounds, such as tholins.[7] The water and methane ices can cover no more than 50% and 30% of the surface, respectively.[25] This means the proportion of ice on the surface is less than on Charon, but similar to that on Triton.[25]

Later in 2008–2010 new infrared spectroscopic observations with a higher signal-to-noise ratio revealed additional spectral features. Among them are a deep water ice absorption band at 1.65 μm, which is an evidence of the crystalline water ice on the surface of Orcus, and a new absorption band at 2.22 μm. The origin of the latter feature is not completely clear. It can be caused either by ammonia/ammonium dissolved in the water ice or by methane/ethane ices.[6] The radiative transfer modeling showed that a mixture of water ice, tholins (as a darkening agent), ethane ice and ammonium ion (NH4+) provides the best match to the spectra, whereas a combination of water ice, tholins, methane ice and ammonia hydrate gives a slightly inferior result. On the other hand, a mixture of only ammonia hydrate, tholins and water ice failed to provide a satisfactory match.[13] So, as of 2010, the only reliably identified compounds on the surface of Orcus are crystalline water ice and, possibly, dark tholins. A firm identification of ammonia, methane and other hydrocarbons requires better infrared spectra.[13]

Comparison with moons and other TNOs

Artistic comparison of Pluto, Eris, Makemake, Haumea, Sedna, 2007 OR10, Quaoar, Orcus, and Earth.
( )

Orcus straddles the edge for trans-Neptunian objects massive enough to retain volatiles such as methane on the surface.[13] The reflectance spectrum of Orcus shows the deepest water-ice absorption bands of any Kuiper belt object (KBO) that is not associated with the Haumea collisional family.[10] The large icy satellites of Uranus have infrared spectra quite similar to that of Orcus.[10] Among other trans-Neptunian objects Pluto's moon Charon appears to be most similar to Orcus. It has a higher albedo but very similar visible and near-infrared spectra. Their densities are also similar and both have water ice rich surfaces.[6] Quaoar—a trans-Neptunian object of similar size—has strong water ice absorption features in its spectra but also has a very red color in the visible line implying the presence of ultrared matter on its surface. Dwarf planet Haumea and objects from its collisional family have much higher albedos and much deeper water absorption bands than Orcus. Finally, (208996) 2003 AZ84—another large object in 2:3 resonance with Neptune—has spectral properties very similar to Orcus.[13]


The presence of crystalline water ice, and possibly ammonia ice may indicate that a renewal mechanism was active in the past on the surface of Orcus.[6] Ammonia so far has not been detected on any TNO or icy satellite of the outer planets other than Miranda.[6] The 1.65 μm band on Orcus is broad and deep (12%), as on Charon, Quaoar, Haumea, and icy satellites of giant planets.[6] On the other hand the crystalline water ice on the surfaces of TNOs should be completely amorphized by the galactic and Solar radiation in about 10 million years.[6] Some calculations indicate that cryovolcanism, which is considered one of the possible renewal mechanisms, may indeed be possible for TNOs larger than about 1000 km.[13] Orcus may have experienced at least one such episode in the past, which turned the amorphous water ice on its surface into crystalline. The preferred type of volcanism may have been explosive aqueous volcanism driven by an explosive dissolution of methane from water–ammonia melts.[13]

Models of internal heating via radioactive decay suggest that Orcus may be capable of sustaining an internal ocean of liquid water.[26]


Vanth could easily be 1/3 to 1/2 the diameter of Orcus

Using observations with the Hubble Space Telescope from November 13, 2005, Mike Brown and T.A. Suer detected a satellite.[27] The discovery of a satellite of Orcus was reported in IAUC 8812 on 22 February 2007.[15] The satellite was given the designation S/2005 (90482) 1 before later being named Vanth. It orbits Orcus in a nearly face-on circular orbit with an eccentricity of about 0.007, and an orbital period of 9.54 days.[10] Vanth orbits only 9030±89 km from Orcus and is too close to Orcus for ground-based spectroscopy to determine the surface composition of the satellite.[5]

Mike Brown suspects that like the Pluto–Charon system, Orcus and Vanth are tidally locked.[11] Vanth does not resemble known collisional satellites because its spectrum is very different from that of its primary, and it may be a captured KBO.[11] Vanth could also have originated as a result of rotational fission of the primordial Orcus, which would have rotated much faster than now.[14]

On March 23, 2009, Brown asked readers of his weekly column to suggest possible names for the satellite, with the best one to be submitted to the International Astronomical Union (IAU) on April 5.[11] The name Vanth, after the Etruscan goddess who guided the souls of the dead to the underworld, was eventually chosen from among a large pool of submissions.[16] This submission was assessed by the IAU's Committee for Small Body Nomenclature, which voted to approve it in March 2010, in accordance with the normal object naming procedures.[28][29]


  1. ^ a b c "JPL Small-Body Database Browser: 90482 Orcus (2004 DW)" (2010-02-09 last obs). Retrieved 2010-12-31. 
  2. ^ a b c  
  3. ^ "MPEC 2009-E53 :Distant Minor Planets (2009 MAR. 30.0 TT)". Minor Planet Center. 2009-03-11. Retrieved 2011-07-05. 
  4. ^ a b c d e f g h i Fornasier,, S.; Lellouch,, E.; Müller, P., T.; et .al. (2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 µm.". Astronomy&Astrophysics 555: A92.  
  5. ^ a b c Carry, B.; Hestroffer, D.; Demeo, F. E.; Thirouin, A.; Berthier, J.; Lacerda, P.; Sicardy, B.; Doressoundiram, A.; Dumas, C.; Farrelly, D.; Müller, T. G. (2011). "Integral-field spectroscopy of (90482) Orcus-Vanth". Astronomy & Astrophysics 534: A115.  
  6. ^ a b c d e f g h i Barucci, M. A.; Merlin; Guilbert; Bergh; Doressoundiram; et al. (2008). "Surface composition and temperature of the TNO Orcus". Astronomy and Astrophysics 479 (1): L13–L16.  
  7. ^ a b de Bergh, C.; A. Delsanti; G. P. Tozzi; E. Dotto; A. Doressoundiram; M. A. Barucci (2005). "The Surface of the Transneptunian Object 9048 Orcus". Astronomy & Astrophysics 437 (3): 1115–1120.  
  8. ^ a b "AstDys (90482) Orcus Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2009-03-19. 
  9. ^ a b "HORIZONS Web-Interface". JPL Solar System Dynamics. Retrieved 2008-07-02. 
  10. ^ a b c d e f g h Brown, M.E.; Ragozzine, D.; Stansberry, J.; Fraser, W.C. (2010). "The size, density, and formation of the Orcus-Vanth system in the Kuiper belt". The Astronomical Journal 139 (6): 2700–2705.  
  11. ^ a b c d e  
  12. ^ "MPEC 2004-D15 : 2004 DW". Minor Planet Center. 2004-02-20. Retrieved 2011-07-05. 
  13. ^ a b c d e f g h A. Delsanti, F. Merlin, A. Guilbert–Lepoutre at al. (2010). "Methane, ammonia, and their irradiation products at the surface of an intermediate-size KBO? A portrait of Plutino (90482) Orcus". Astronomy and Astrophysics 627 (2): 1057.  
  14. ^ a b c d Ortiz, J. L.; Cikota, A.; Cikota, S.; Hestroffer, D.; Thirouin, A.; Morales, N.; Duffard, R.; Gil-Hutton, R.; Santos-Sanz, P.; De La Cueva, I. (2010). "A mid-term astrometric and photometric study of trans-Neptunian object (90482) Orcus". Astronomy & Astrophysics 525: A31.  
  15. ^ a b c Wm. Robert Johnston (2007-03-04). "(90482) Orcus". Johnston's Archive. Archived from the original on 10 February 2009. Retrieved 2009-03-26. 
  16. ^ a b  
  17. ^ Stansberry, J.; Grundy, W.; Brown, M.; Cruikshank, D.; Spencer, J.; Trilling, D.; Margot, J.-L. (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope". In M. A. Barucci; H. Boehnhardt; D. P. Cruikshank; A. Morbidelli. The Solar System Beyond Neptune. Tucson: University of Arizona Press. pp. 161–179.  
  18. ^ Wm. Robert Johnston (2008-09-17). "TNO/Centaur diameters and albedos". Johnston's Archive. Archived from the original on 22 October 2008. Retrieved 2008-10-17. 
  19. ^  
  20. ^ Tancredi, G.; Favre, S. (2008). "Which are the dwarfs in the solar system?" (PDF). Asteroids, Comets, Meteors. Retrieved 2007-12-28. 
  21. ^ O. Gingerich (2006). "The Path to Defining Planets" (PDF). Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair. Retrieved 2007-03-13. 
  22. ^ "Planetary Names: Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. International Astronomical Union (Working Group for Planetary System Nomenclature). Retrieved 10 June 2012. 
  23. ^ NASA. "List of Dwarf Planets". Retrieved 2012-06-09. 
  24. ^ Fornasier, S.; Dotto, E.; Barucci, M.A.; Barbieri, C. (2004). "Water ice on the surface of the large TNO 2004 DW". Astronomy & Astrophysics 422 (2): L43–L46.  
  25. ^ a b  
  26. ^ Hussmann, Hauke; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects" (PDF).  
  27. ^ Daniel W. E. Green (2007-02-22). "IAUC 8812: Sats OF 2003 AZ_84, (50000), (55637), (90482)". International Astronomical Union Circular. Archived from the original on 19 July 2011. Retrieved 2011-07-05. 
  28. ^ "Committee on Small Body Nomenclature: Names of Minor Planets". Retrieved 2009-04-08. 
  29. ^

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