(225088) 2007 OR10

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(225088) 2007 OR10
Discovery[1]
Discovered by
Discovery date 17 July 2007 [a]
Designations
MPC designation (225088) 2007 OR10
SDO[2]
3:10 resonance (DES)[3]
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 10989 days (30.09 yr)
Aphelion 100.84 AU (15.085 Tm) (Q)
Perihelion 33.015 AU (4.9390 Tm) (q)
66.925 AU (10.0118 Tm) (a)
Eccentricity 0.50669 (e)
547.51 yr (199978 d)
104.15° (M)
0° 0m 6.481s / day (n)
Inclination 30.9434° (i)
336.8141° (Ω)
206.81° (ω)
Earth MOID 32.0462 AU (4.79404 Tm)
Jupiter MOID 27.7579 AU (4.15252 Tm)
Jupiter Tisserand parameter 5.381
Physical characteristics
Dimensions 1535+75
−225
 km
[5]
1280+210
−210
 km
[6]
1200+300
−200
 km
[7][b]
Mass ~1.3–6 × 1021 kg (estimate)
44.81 h[5]
0.089+0.031
−0.009
[5] 0.185+0.076
−0.052
[6]
Temperature 31 K[8]
red[7]
21.8[9]
2.5[4]

(225088) 2007 OR10 is a large scattered disc object. It is the third-largest known body in the Solar System beyond Neptune,[5][10][11] and the largest known body in the Solar System without a name.[12] According to current estimates as of May 2016, it is slightly larger than Makemake or Haumea, and is hence probably a dwarf planet.

History[edit]

Discovery[edit]

(225088) 2007 OR10 was discovered by California Institute of Technology astronomers as part of the PhD thesis of Meg Schwamb, who was at the time a graduate student of Michael E. Brown.[13]

Naming[edit]

Brown nicknamed the object "Snow White" for its presumed white color,[13] because it would have to be very large or very bright to be detected by their survey.[12] It was also the "seventh dwarf" discovered by Brown's team, after Quaoar in 2002, Sedna in 2003, Haumea and Orcus in 2004, and Makemake and Eris in 2005. However, 2007 OR10 turned out to be one of the reddest objects in the Kuiper belt, comparable only to Quaoar, so the nickname was dropped.

2007 OR10 is currently the largest known object in the Solar System without an official name. In 2011 Brown decided he finally had enough information to justify giving it one, because the discovery of water ice and the possibility of methane makes it noteworthy enough to warrant further study.[13] However, as of 2015, Brown had yet to propose a name, though he notes that in 2017 anyone will be able to make a proposal.[14]

Distance[edit]

(225088) 2007 OR10 came to perihelion around 1857.[4] As of February 2016 it is located 87.5 AU from the Sun[15] and moving at 2.7 kilometers per second (6,000 miles per hour) with respect to the Sun.[16] This makes it the third-farthest known large body in the Solar System, after V774104 (103 AU) and Eris (96.3 AU), and farther out than Sedna (85.7 AU).[12] It has been farther from the Sun than Sedna since 2013.[16] 2007 OR10 will be farther than both Sedna and Eris by 2045,[17] and it will reach aphelion in 2130.[16]

Most-distant known objects in the
Solar System as of 7 June 2016[15]
Object name Distance from the Sun (AU) Magnitude
(vmag)
Current Perihelion Aphelion
V774104 103 N/A N/A 24
Eris 96.3 37.8 97.6 18.7
2007 OR10 87.5 33.0 100.8 21.7
Sedna 85.7 76.0 939 21.0
2014 FC69 84.2 40.3 106.9 24.1
2006 QH181 83.5 37.8 96.7 23.6
2012 VP113 83.4 80.5 438 23.4
2013 FY27 80.2 36.1 81.8 22.1
2010 GB174 70.9 48.7 693 25.1
2012 FH84 68.5 45.8 80.6 25.7
2015 GP50 67.9 35.9 89.1 24.8
2013 FQ28 67.4 48.7 80.6 24.4
2015 RR245 64.1 33.7 129.2 22.1
2000 CR105 60.6 44.3 412 23.9
2008 ST291 59.9 42.4 154.5 22.2
2003 QX113 59.9 36.7 62.1 22.5
2015 KH162 59.1 41.5 82.8 21.6
Including all known objects currently located at least twice as far as Neptune.[15]
See List of trans-Neptunian objects for more.

Absolute magnitude[edit]

The size of an object can be calculated from its absolute magnitude (H) and the albedo (the amount of light it reflects). 2007 OR10 has an absolute magnitude (H) of 1.92,[4] which makes it the fifth-brightest TNO known,[18] a little less bright than Sedna (H=1.6; D≈1,000 km)[19] and brighter than Orcus (H=2.3; D≈800 km).[20]

2007 OR10 is among the reddest objects known.[7] This is probably in part due to methane frosts, which turn red when bombarded by sunlight and cosmic rays.[7]

Surface composition and atmosphere[edit]

The spectrum of 2007 OR10 shows signatures for both water ice and methane, which makes it similar in composition to Quaoar. The presence of red methane frost on the surfaces of both 2007 OR10 and Quaoar implies the existence of a tenuous methane atmosphere on both objects, slowly evaporating into space. Although 2007 OR10 comes closer to the Sun than Quaoar, and is thus warm enough that a methane atmosphere should evaporate, its larger mass makes retention of an atmosphere just possible.[7] In particular, 2007 OR10's large size means that it is likely to retain even nitrogen, which almost all TNOs lose over the course of their existence.[21] The presence of water ice on the surface of 2007 OR10 implies a brief period of cryovolcanism in its distant past.[22]

Orbit[edit]

Earth Moon Dysnomia Dysnomia Eris Eris Charon Charon Nix Nix Kerberos Kerberos Styx Styx Hydra Pluto Pluto Makemake Makemake Namaka Namaka Hi'iaka Hi'iaka Haumea Haumea Sedna Sedna 2007 OR10 2007 OR10 Weywot Weywot Quaoar Quaoar Vanth Vanth Orcus Orcus File:EightTNOs.png
Artistic comparison of Pluto, Eris, Makemake, Haumea, Sedna, 2007 OR10, Quaoar, Orcus, and Earth along with the Moon.

The Deep Ecliptic Survey (DES) shows the orbit to be in a 3:10 resonance with Neptune.[3] The MPC lists it as a scattered-disc object.[2] 2007 OR10 was discovered when searching for objects in the region of Sedna.[23]

2007 OR10 has been observed 46 times over seven oppositions with a precovery image from 1985.[4]

It was formally announced on 7 January 2009.[1]

The orbit of 2007 OR10 compared to the orbit of Eris, Pluto, and the outer planets
Resonance. The motion of 2007 OR10 librating in a 3:10 resonance with Neptune.[3] Neptune is held stationary.

Dwarf-planet status[edit]

Based on the most recent size estimates as of May 2016,[5] 2007 OR10 would be the third-largest dwarf planet, after Pluto and Eris, and before Makemake, Haumea, and Ceres, though the error bars overlap with those of Makemake. The IAU has not addressed the possibility of accepting additional dwarf planets since before the discovery of 2007 OR10 was announced. Brown states that it "must be a dwarf planet even if predominantly rocky",[24] and Scott Sheppard and colleagues think that it is "likely" to be a dwarf planet,[25] based on its minimum possible diameter (552 km)[26] and what is understood of the conditions for hydrostatic equilibrium in cold icy–rocky bodies. 2007 OR10 is too distant for its diameter to be resolved directly; Brown's estimate of 1,000–1,500 km is based on calculating the albedo that is the best fit in his model,[7] which agrees with the 1280±210 km determined from observations by the Herschel space observatory.[6] 2007 OR10 has no known satellite, and without a satellite with a well-determined orbit, its mass cannot be calculated directly; mass is also a factor in hydrostatic equilibrium.

See also[edit]

Notes[edit]

  1. ^ discovery was announced two years later on 7 January 2009
  2. ^ dimension: fit to volatile-retention model

References[edit]

  1. ^ a b "MPEC 2009-A42 : 2007 OR10". Minor Planet Center. 7 January 2009. Archived from the original on 11 March 2012. 
  2. ^ a b "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 20 January 2009. 
  3. ^ a b c Marc Buie (24 October 2011). "Orbit Fit and Astrometric record for 225088". SwRI (Space Science Department). Retrieved 14 November 2014. 
  4. ^ a b c d e "JPL Small-Body Database Browser: 225088 (2007 OR10)" (2011-10-24). Retrieved 7 April 2016. last obs; arc: 26.18 years 
  5. ^ a b c d e "Pushing the Limits of K2:Observing Trans-Neptunian Objects S3K2: Solar System Studies with K2" (PDF). 
  6. ^ a b c Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; Pal, A.; Müller, T.G.; Vilenius, E.; Stansberry, J.; Mommert, M.; Delsanti, A.; Mueller, M.; Peixinho, N.; Henry, F.; Ortiz, J.L.; Thirouin, A.; Protopapa, S.; Duffard, R.; Szalai, N.; Lim, T.; Ejeta, C.; Hartogh, P.; Harris, A.W.; Rengel, M. (7 February 2012). ""TNOs are Cool": A Survey of the Transneptunian Region IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS". arXiv:1202.1481v1 [astro-ph.EP]. 
  7. ^ a b c d e f Michael E. Brown; Burgasser, A.J.; Fraser W.C. (2011). "The Surface Composition of Large Kuiper Belt Object 2007 OR10" (PDF). The Astrophysical Journal Letters (Mike Brown's Website) 738 (2): L26. arXiv:1108.1418. Bibcode:2011ApJ...738L..26B. doi:10.1088/2041-8205/738/2/L26. Retrieved 8 August 2011. 
  8. ^ "HEC: Exoplanets Calculator". Planetary Habitability Laboratory. University of Puerto Rico at Arecibo. Retrieved 17 October 2014. 
  9. ^ "AstDys 2007OR10 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 17 May 2009. Retrieved 16 March 2009. 
  10. ^ Pál, A.; Kiss, C.; Müller, T. G.; Molnár, L.; Szabó, R.; Szabó, G. M.; Sárneczky, K.; Kiss, L. L. (2016-04-19). "Large size and slow rotation of the trans-Neptunian object (225088) 2007 OR10 discovered from Herschel and K2 observations". The Astronomical Journal 151 (5): 117. doi:10.3847/0004-6256/151/5/117. 
  11. ^ Dyches, P. (2016-05-11). "2007 OR10: Largest Unnamed World in the Solar System". Jet Propulsion Lab. Retrieved 2016-05-12. 
  12. ^ a b c Michael E. Brown (10 March 2009). "Snow White needs a bailout". Mike Brown's Planets (blog). Archived from the original on 17 May 2009. Retrieved 17 February 2010. 
  13. ^ a b c "Astronomers Find Ice and Possibly Methane On Snow White, a Distant Dwarf Planet". Science Daily. 22 August 2011. Retrieved 22 August 2011. 
  14. ^ "Mike Brown's Planets". mikebrownsplanets.com. 
  15. ^ a b c "AstDyS-2, Asteroids - Dynamic Site". 2016-02-26. Retrieved 2016-02-29. Objects with distance from Sun over 59 AU 
  16. ^ a b c "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. Retrieved 31 January 2012. 
  17. ^ JPL Horizons On-Line Ephemeris System (17 February 2011). "Horizons Output for Sedna 2076/2114". Retrieved 17 February 2011. 
  18. ^ Brown, Mike Brown (11 August 2011). "The Redemption of Snow White (Part 2 of 3)". Mike Brown's Planets. Archived from the original on 25 July 2014. 
  19. ^ "JPL Small-Body Database Browser: 90377 Sedna (2003 VB12)" (2008-10-23 last obs). Retrieved 21 January 2009. 
  20. ^ "JPL Small-Body Database Browser: 90482 Orcus (2004 DW)" (2008-12-04 last obs). Retrieved 5 February 2009. 
  21. ^ http://www.jpl.nasa.gov/news/news.php?feature=6509
  22. ^ Brown, Mike (20 August 2011). "The Redemption of Snow White (Part 3 of 3)". Mike Brown's Planets. Archived from the original on 25 July 2014. 
  23. ^ Schwamb, Megan E.; Brown, Michael E.; Rabinowitz, David L. (2009). "A Search for Distant Solar System Bodies in the Region of Sedna". Astrophysical Journal Letters 694: L45. arXiv:0901.4173. Bibcode:2009ApJ...694L..45S. doi:10.1088/0004-637X/694/1/L45. 
  24. ^ Brown, Michael E. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 23 September 2011. 
  25. ^ Sheppard, Scott S.; Udalski, Andrezej; Trujillo, Chadwick; et al. (2011). "A Southern Sky and Galactic Plane Survey for Bright Kuiper Belt Objects". Astronomical Journal 142 (4): 98. arXiv:1107.5309. Bibcode:2011AJ....142...98S. doi:10.1088/0004-6256/142/4/98. 
  26. ^ 1329×10(−H/5)

External links[edit]