(90568) 2004 GV 9

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Asteroid
(90568) 2004 GV 9
Image taken by the Hubble Space Telescope
Image taken by the Hubble Space Telescope
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type DO (E SDO ), or
CKBO ( «Hot» )
«Distant Object»
Major semi-axis 42.218  AU
eccentricity 0.08
Perihelion - aphelion 38.838 AU - 45.599 AU
Inclination of the orbit plane 21.9 °
Length of the ascending node 250.7 °
Argument of the periapsis 295.9 °
Time of passage of the perihelion June 15, 1991
Sidereal period 274 a 3.8 M
Mean orbital velocity 4.547 km / s
Physical Properties
Medium diameter
Albedo
Rotation period 5.86 ± 0.03 h (0.244 d )
Absolute brightness 4.23 ± 0.1 mag
Spectral class C
B-V = 0.730 ± 0.010
VR = 0.630 ± 0.010
VI = 1.510 ± 0.014
BR = 1.470 ± 0.030
history
Explorer NEAT :
Steven H. Pravdo
Daniel MacDonald
Kenneth J. Lawrence
Michael Hicks
Date of discovery April 13, 2004
Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . The affiliation to an asteroid family is automatically determined from the AstDyS-2 database . Please also note the note on asteroid items.

(90568) 2004 GV 9 is a large trans-Neptunian object in the Kuiper belt , which is classified as an extended Scattered Disk Object (DO) or as a Cubewano (CKBO) in terms of orbital dynamics. Because of its size, the asteroid is a dwarf planet candidate .

discovery

(90568) 2004 GV 9 was discovered on April 13, 2004 by a team of astronomers consisting of Steven Pravdo, Daniel MacDonald, Kenneth Lawrence and Michael Hicks as part of Near Earth Asteroid Tracking at the 1.2 m Oschin Schmidt telescope of the Discovered at Palomar Observatory, California . The discovery was announced on April 14, 2004, and the planetoid was later given the minor planet number 90568 by the IAU .

After its discovery, GV 9 could be identified back in 2004 on photos of December 21, 1954, which were also taken at the Palomar Observatory as part of the Digitized Sky Survey program, and thus its observation period was extended by 50 years, thus extending its orbit to calculate more precisely. Since then, the planetoid has been observed through various telescopes such as the Herschel and Spitzer space telescopes as well as earth-based telescopes. In November 2017, a total of 125 observations were made over a period of 61 years. The last observation so far was carried out in June 2018 at the Vegaquattro Observatory ( Piedmont ). (As of March 12, 2019)

properties

Orbit

2004 GV 9 orbits the sun in 274.32 years in an almost circular orbit between 38.84  AU and 45.60 AU from its center. The orbit eccentricity is 0.080, the orbit is inclined 21.92 ° with respect to the ecliptic . The planetoid is currently 39.61 AU from the Sun. The last time he passed through perihelion was in 1991, so the next perihelion should take place in 2265.

Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center does not have a specific classification; the latter classifies it as a non-SDO and generally as a “distant object” . The Johnston's Archive, however, lists him as Cubewano , whereby he would belong to the "hot" classic KBO in terms of rail dynamics .

Size and rotation

With the Spitzer space telescope, a diameter of 677 ± 70 km was determined in 2007. Combined with the data from the Herschel space telescope, it was refined to 680 ± 34 km in 2012. Based on the latter diameter, the total surface area is around 1,453,000 km². The apparent magnitude of 2005 RN 43 is 20.00  m .

Since it can be assumed that 2004 GV 9 is in hydrostatic equilibrium due to its size and must therefore be largely round, it should meet the criteria for classification as a dwarf planet . Mike Brown assumes that 2004 GV 9 is most likely a dwarf planet, Gonzalo Tancredi also accepted it as a possible dwarf planet in 2010, but did not propose to the IAU to officially recognize it as such.

Using light curve observations , 2004 GV 9 rotates once around its axis in 5 hours and 51.6 minutes. It follows that in a 2004 GV 9 year it performs 410,356.5 self- rotations (“days”). However, this is still fraught with uncertainties, as the observation time at that time was insufficient and the error rate is around 30%.

Provisions of the diameter for 2004 GV 9
year Dimensions km source
2007 677.2 +71.3−69.3 Stansberry et al. a.
2008 636.0 Tancredi
2008 684.0 +68.0−78.0 Brucker et al. a.
2010 677.0 Tancredi
2012 680.0 ± 34.0 Vilenius et al. a.
2018 730.34 LightCurve DataBase
2018 703.0 Brown
The most precise determination is marked in bold .

See also

Web links

Commons : (90568) 2004 GV9  - Collection of Images, Videos and Audio Files

Individual evidence

  1. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 90568 . SwRI (Space Science Department). Retrieved March 12, 2019.
  2. ^ A b Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 12, 2019.
  3. ↑ a b c (90568) 2004 GV9 at the IAU Minor Planet Center (English) Retrieved on March 12, 2019.
  4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  5. ↑ a b c d e E. Vilenius u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel / PACS observations and thermal modeling of 19 classical Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 541, No. A94, April 4, 2012, p. 17. arxiv : 1204.0697 . bibcode : 2012A & A ... 541A..94V . doi : 10.1051 / 0004-6361 / 201118743 .
  6. ↑ D. Perna et al. a .: Light Curves and Densities of Centaurs and Trans-Neptunian Objects from the ESO Large Program . In: American Astronomical Society, DPS meeting . 40, September 2008, p. 483. bibcode : 2008DPS .... 40.4708P .
  7. ↑ a b LCDB Data for (90568) 2004GV9 . MinorPlanetInfo. 2018. Retrieved March 12, 2019.
  8. ↑ a b c H. Boehnhardt u. a .: Photometry of Transneptunian Objects for the Herschel Key Program “TNOs are Cool” . In: Earth, Moon, and Planets . 114, No. 1-2, November 2014, pp. 35-57. bibcode : 2014EM & P..114 ... 35B . doi : 10.1007 / s11038-014-9450-x .
  9. ↑ S. Tegler u. a .: Two Color Populations of Kuiper Belt and Centaur Objects and the Smaller Orbital Inclinations of Red Centaur Objects (PDF) . In: The Astronomical Journal . 152, No. 6, December 2016, p. 210, 13. bibcode : 2016AJ .... 152..210T . doi : 10.3847 / 0004-6256 / 152/6/210 .
  10. ↑ MPC : MPEC 2004-G32: 2004 GV9 . IAU . April 14, 2004. Retrieved March 12, 2019.
  11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 12, 2019.
  12. ↑ (90568) 2004 GV9 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 12, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  13. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . March 12, 2010. Accessed March 12, 2019.
  14. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 12, 2019.
  15. ↑ (90568) 2004 GV9 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  16. ^ A b G. Tancredi: Physical and dynamical characteristics of icy “dwarf planets” (plutoids) (PDF) . In: International Astronomical Union (Ed.): Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009 . 2010. doi : 10.1017 / S1743921310001717 . Retrieved March 12, 2019.
  17. ↑ J. Stansberry et al. a .: Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope (PDF) . In: University of Arizona Press . 592, No. 161-179, February 20, 2007. arxiv : astro-ph / 0702538 . bibcode : 2008ssbn.book..161S .
  18. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . August. Retrieved March 12, 2019.
  19. ↑ M. Brucker et al. a .: High Albedos of Low Inclination Classical Kuiper Belt Objects (PDF) . In: Icarus . January 1, 2009, p. 26. arxiv : 0812.4290 . bibcode : 2012A & A ... 546A..86P . doi : 10.1016 / j.icarus.2008.12.040 .
  20. ↑ Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 12, 2019.