Orcus and its moon Vanth imaged by the Hubble Space Telescope in 2006
|Discovered by||M. E. Brown|
|Discovery date||17 February 2004|
|Orcus (Roman mythology)|
|TNO  · plutino |
possible dwarf planet 
|Orbital characteristics |
|Epoch 31 May 2020 (JD 2459000.5)|
|Uncertainty parameter 2|
|Observation arc||68.16 yr (24,894 days)|
|Earliest precovery date||8 November 1951|
|Aphelion||48.067 AU (7.1907 Tm)|
|Perihelion||30.281 AU (4.5300 Tm)|
|39.174 AU (5.8603 Tm)|
|245.19 yr (89,557 days)|
|0° 0m 14.472s / day|
|≈ 9 January 2143|
−40 km 917±25 km
|Mass||(6.348±0.019)×1020 kg (system)|
Equatorial surface gravity
|≈ 0.2 m/s2|
Equatorial escape velocity
|≈ 0.43 km/s|
|Temperature||< 44 K|
V–R = 0.37
|2.31±0.03 (integral), 2.41±0.05|
90482 Orcus, provisional designation 2004 DW, is a trans-Neptunian object with a large moon, Vanth. With a diameter of 910 km (570 mi), it is a possible dwarf planet. The surface of Orcus is relatively bright with albedo reaching 23 percent, neutral in color and rich in water ice. 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 on its surface. It was discovered by American astronomers Michael Brown, Chad Trujillo, and David Rabinowitz on 17 February 2004.
Orcus is a plutino, a trans-Neptunian object that is locked in a 2:3 resonance with the ice giant Neptune, making two revolutions around the Sun to every three of Neptune's. This is much like Pluto, except that the phase of Orcus' orbit is opposite from Pluto's: Orcus is at aphelion when Pluto is at perihelion and vice versa. Moreover, the aphelion of Orcus' 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.
Orcus was discovered on 17 February 2004, by American astronomers Michael Brown of Caltech, Chad Trujillo of the Gemini Observatory, and David Rabinowitz of Yale University. Precovery images taken by the Palomar Observatory as early as 8 November 1951 were later obtained from the Digitized Sky Survey.
The minor planet Orcus was named after one of the Roman gods of the underworld, Orcus. While Pluto was the ruler of the underworld, Orcus was a punisher of the condemned. The approved naming citation was published by the Minor Planet Center on 26 November 2004 (M.P.C. 53177). Under the guidelines of the International Astronomical Union's (IAU) 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. The name was also a private reference to the homonymous Orcas Island, where Brown's wife had lived as a child and that they visit frequently.
On 30 March 2005, Orcus's moon, 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 psychopomp, a guide of the deceased to the underworld.
Size and magnitude
The absolute magnitude of Orcus is approximately 2.3. The detection of Orcus by the Spitzer Space Telescope in the far infrared and by Herschel Space Telescope in submillimeter estimates its diameter at 958.4 km (595.5 mi), with an uncertainty of 22.9 km (14.2 mi). Orcus appears to have an albedo of about 21–25 percent, which may be typical of trans-Neptunian objects approaching the 1,000 km (620 mi) diameter range. The magnitude and size estimates were made under the assumption that Orcus is a singular object. The presence of a relatively large satellite, Vanth, 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. The ALMA submillimeter measurements taken in 2016 showed that Vanth has a relatively large size of 475 km (295 mi) with albedo of about 8 percent while Orcus's has a slightly smaller size of 910 km (570 mi). Using a stellar occultation by Vanth in 2017, Vanth's diameter has been determined to be 442.5 km (275.0 mi), with an uncertainty of 10.2 km (6.3 mi). Michael Brown's website lists Orcus as a dwarf planet with "near certainty", Tancredi concludes that it is one, and is massive enough to be considered one under the 2006 draft proposal of the IAU, but the IAU has not formally recognized it as such.
Mass and density
Orcus and Vanth are known to constitute a binary system. The mass of the system has been estimated to be (6.348±0.019)×1020 kg, approximately equal to that of the Saturnian moon Tethys (6.175×1020 kg). Compared to the most massive known dwarf planet, Eris, the mass of the Orcus system is about 3.8 percent that of Eris (1.66×1022 kg). How this mass is partitioned between Orcus and Vanth depends on their relative densities. While Orcus is known to have a density of about 1.53 g/cm3, the density of Vanth is uncertain, with estimates ranging from 1.53 g/cm3, to 0.8 g/cm3.
Spectra and surface
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. The neutral visible spectrum and strong water absorption bands of Orcus showed that Orcus appeared different from other trans-Neptunian objects, which typically have a red visible spectrum and often featureless infrared spectra. Further infrared observations in 2004 by the European Southern Observatory and the Gemini telescope gave results consistent with mixtures of water ice and carbonaceous compounds, such as tholins. The water and methane ices can cover no more than 50 percent and 30 percent of the surface, respectively. This means the proportion of ice on the surface is less than on Charon, but similar to that on Triton.
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. 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. 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.
Orcus sits at the threshold for trans-Neptunian objects massive enough to retain volatiles such as methane on the surface. The reflectance spectrum of Orcus shows the deepest water-ice absorption bands of any Kuiper belt object that is not associated with the Haumea collisional family. The large icy satellites of Uranus have infrared spectra quite similar to that of Orcus. Among other trans-Neptunian objects, the large plutino 2003 AZ84 and Pluto's moon Charon both have similar surface spectra to Orcus, with flat, featureless visible spectra and moderately strong water ice absorption bands in the near-infrared.
Crystalline water ice on the surfaces of trans-Neptunian objects should be completely amorphized by the galactic and Solar radiation in about 10 million years. Thus 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. Ammonia so far has not been detected on any trans-Neptunian object or icy satellite of the outer planets other than Miranda. The 1.65 μm band on Orcus is broad and deep (12%), as on Charon, Quaoar, Haumea, and icy satellites of giant planets. Some calculations indicate that cryovolcanism, which is considered one of the possible renewal mechanisms, may indeed be possible for trans-Neptunian objects larger than about 1,000 km (620 mi). 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. Models of internal heating via radioactive decay suggest that Orcus may be capable of sustaining an internal ocean of liquid water.
Orbit and rotation
Orcus is in a 2:3 orbital resonance with Neptune, having an orbital period of 245 years, and is classified as a plutino. Its orbit is moderately inclined at 20.6 degrees to the ecliptic. 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. 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". Orcus last reached its aphelion (farthest distance from the Sun) in 2019 and will come to perihelion (closest distance to the Sun) around 9 January 2143. Simulations by the Deep Ecliptic Survey show that over the next 10 million years Orcus may acquire a perihelion distance (qmin) as small as 27.8 AU.
The rotation period of Orcus is uncertain, as 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. The rotational axis of Orcus probably coincides with the orbital axis 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. Astronomer José Luis Ortiz and colleagues have derived a possible rotation period of about 10.5 hours, assuming that Orcus is not tidally locked with Vanth. If, however, the primary is tidally locked with the satellite, the rotational period would coincide with the 9.7-day orbital period of Vanth.
Orcus has one known moon, Vanth (full designation (90482) Orcus I Vanth). It was discovered by Michael Brown and T.-A. Suer using discovery images taken by the Hubble Space Telescope on 13 November 2005. The discovery was announced in an IAU Circular notice published on 22 February 2007. A spatially resolved submillimeter imaging of Orcus–Vanth system in 2016 showed that Vanth has a relatively large size of 475 km (295 mi), with an uncertainty of 75 km (47 mi). That estimate for Vanth is in good agreement with the size of about 442.5 km (275.0 mi) derived from a stellar occultation in 2017. Like Charon compared to Pluto, Vanth is quite large compared to Orcus, and is one reason for characterizing Orcus as the 'anti-Pluto'. If Orcus is a dwarf planet, Vanth would be the third-largest known dwarf-planet moon, after Charon and Dysnomia. The ratio of masses of Orcus and Vanth is uncertain, possibly anywhere from 1:33 to 1:12.
- "JPL Small-Body Database Browser: 90482 Orcus (2004 DW)" (2020-01-04 last obs.). Jet Propulsion Laboratory. 29 January 2020. Retrieved 20 February 2020.
- "90482 Orcus (2004 DW)". Minor Planet Center. Retrieved 3 April 2017.
- Schmadel, Lutz D. (2006). "(90482) Orcus [39.5, 0.22, 20.5]". Dictionary of Minor Planet Names – (90482) Orcus, Addendum to Fifth Edition: 2003–2005. Springer Berlin Heidelberg. p. 236. doi:10.1007/978-3-540-34361-5_2818. ISBN 978-3-540-34361-5.
- Buie, Marc W. (22 December 2007). "Orbit Fit and Astrometric record for 90482". SwRI (Space Science Department). Retrieved 19 September 2008.
- "MPEC 2009-E53 :Distant Minor Planets (2009 MAR. 30.0 TT)". Minor Planet Center. 11 March 2009. Retrieved 5 July 2011.
- Michael E. Brown (23 Sep 2011). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 18 October 2011. Retrieved 23 September 2011.
- "Orcus". Dictionary.com Unabridged. Random House.
- Angley (1847) De Clifford, the philosopher
- JPL Horizons Observer Location: @sun (perihelion occurs when deldot changes from negative to positive)
- Brown, Michael E.; Butler, Bryan J. (22 January 2018). "Medium-sized satellites of large Kuiper belt objects". The Astronomical Journal. 156 (4): 164. arXiv:1801.07221. doi:10.3847/1538-3881/aad9f2.
- 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. arXiv:1305.0449v2. Bibcode:2013A&A...555A..15F. doi:10.1051/0004-6361/201321329.
- Grundy, W. M.; Noll, K. S.; Roe, H. G.; Buie, M. W.; Porter, S. B.; Parker, A. H.; Nesvorný, D.; Benecchi, S. D.; Stephens, D. C.; Trujillo, C. A. (2019). "Mutual Orbit Orientations of Transneptunian Binaries" (PDF). Icarus. 334: 62–78. Bibcode:2019Icar..334...62G. doi:10.1016/j.icarus.2019.03.035. ISSN 0019-1035. Retrieved 2019-11-13.
- 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. Bibcode:2008A&A...479L..13B. doi:10.1051/0004-6361:20079079.
- 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. Bibcode:2005A&A...437.1115D. doi:10.1051/0004-6361:20042533.
- "HORIZONS Web-Interface". JPL Solar System Dynamics. Retrieved 2 July 2008.
- 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. arXiv:0910.4784. Bibcode:2010AJ....139.2700B. doi:10.1088/0004-6256/139/6/2700.
- "MPEC 2004-D15 : 2004 DW". Minor Planet Center. 20 February 2004. Retrieved 5 July 2011.
- Michael E. Brown (23 March 2009). "S/2005 (90482) 1 needs your help". Mike Brown's Planets (blog). Archived from the original on 28 March 2009. Retrieved 25 March 2009.
- "Distant Planetoid". solarsystem.nasa.gov. NASA. Retrieved 18 May 2019.
- "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 3 April 2017.
- Michael E. Brown (6 April 2009). "Orcus Porcus". Mike Brown's Planets (blog). Archived from the original on 14 April 2009. Retrieved 6 April 2009.
- Wm. Robert Johnston (4 March 2007). "(90482) Orcus". Johnston's Archive. Archived from the original on 10 February 2009. Retrieved 26 March 2009.
- 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 (eds.). The Solar System Beyond Neptune. Tucson: University of Arizona Press. pp. 161–179. Bibcode:2008ssbn.book..161S. ISBN 978-0816527557.
- Wm. Robert Johnston (17 September 2008). "TNO/Centaur diameters and albedos". Johnston's Archive. Archived from the original on 22 October 2008. Retrieved 17 October 2008.
- Sickafoose, A.A.; Bosh, A.S.; Levine, S.E.; Zuluaga, C.A.; Genade, A.; Schindler, K.; Lister, T.A.; Person, M.J. (21 October 2018). "A stellar occultation by Vanth, a satellite of (90482) Orcus". Icarus. 319: 657–668. arXiv:1810.08977. Bibcode:2019Icar..319..657S. doi:10.1016/j.icarus.2018.10.016.
- Tancredi, G.; Favre, S. (2008). "Which are the dwarfs in the solar system?" (PDF). Asteroids, Comets, Meteors. Retrieved 28 December 2007.
- Gingerich, Owen (16 August 2006). "The Path to Defining Planets" (PDF). Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair. p. 4. Retrieved 13 March 2007.
- "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.
- NASA. "List of Dwarf Planets". Archived from the original on 4 May 2012. Retrieved 9 June 2012.
- Jacobson, R. A.; Antreasian, P. G.; Bordi, J. J.; Criddle, K. E.; Ionasescu, R.; Jones, J. B.; Mackenzie, R. A.; Meek, M. C.; Parcher, D.; Pelletier, F. J.; Owen, Jr., W. M.; Roth, D. C.; Roundhill, I. M.; Stauch, J. R. (December 2006). "The Gravity Field of the Saturnian System from Satellite Observations and Spacecraft Tracking Data". The Astronomical Journal. 132 (6): 2520–2526. Bibcode:2006AJ....132.2520J. doi:10.1086/508812.
- Brown, Michael E.; Schaller, Emily L. (15 June 2007). "The Mass of Dwarf Planet Eris" (PDF). Science. 316 (5831): 1585. Bibcode:2007Sci...316.1585B. doi:10.1126/science.1139415. PMID 17569855. Archived from the original (PDF) on 4 March 2016.
- 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. Bibcode:2004A&A...422L..43F. doi:10.1051/0004-6361:20048004.
- Trujillo, Chadwick A.; Brown, Michael E.; Rabinowitz, David L.; Geballe, Thomas R. (2005). "Near‐Infrared Surface Properties of the Two Intrinsically Brightest Minor Planets: (90377) Sedna and (90482) Orcus". The Astrophysical Journal. 627 (2): 1057–1065. arXiv:astro-ph/0504280. Bibcode:2005ApJ...627.1057T. doi:10.1086/430337.
- A. Delsanti; F. Merlin; A. Guilbert–Lepoutre; et 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. arXiv:1006.4962. Bibcode:2010A&A...520A..40D. doi:10.1051/0004-6361/201014296.
- Hussmann, Hauke; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects". Icarus. 185 (1): 258–273. Bibcode:2006Icar..185..258H. doi:10.1016/j.icarus.2006.06.005.
- 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. arXiv:1010.6187. Bibcode:2011A&A...525A..31O. doi:10.1051/0004-6361/201015309.
- Daniel W. E. Green (22 February 2007). "IAUC 8812: Sats OF 2003 AZ_84, (50000), (55637),, (90482)". International Astronomical Union Circular. Retrieved 4 July 2011.
- Wm. Robert Johnston (4 March 2007). "(90482) Orcus". Johnston's Archive. Retrieved 26 March 2009.
- 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. arXiv:1108.5963. Bibcode:2011A&A...534A.115C. doi:10.1051/0004-6361/201117486.
|Wikimedia Commons has media related to 90482 Orcus.|
- MPEC 2004-D09 announcing the discovery but attributing it to Raymond J. Bambery, Steven H. Pravdo, Michael D. Hicks, Kenneth J. Lawrence, Daniel MacDonald, Eleanor Helin and Robert Thicksten / NEAT
- MPEC 2004-D13 correcting MPEC 2004-D09
- Chad Trujillo's page on 2004 DW
- Orcus of the Outer Solar System, Astronomy Picture of the Day, 25 March 2009
- New world found far beyond Pluto, David Whitehouse, BBC News, 3 March 2004
- A New Kuiper Belt Giant, Stuart Goldman, Sky & Telescope, 24 February 2004
- 90482 Orcus at the JPL Small-Body Database