(19308) 1996 TO 66

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Asteroid
(19308) 1996 TO 66
(19308) 1996 TO66 imaged by NTT cut out.jpg
1996 TO 66 (center above) by the NTT (1998).
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type DO (E SDO ) or
CKBO ( «Hot» ),
«Distant Object»
family Haumea family
Major semi-axis 43.235  AU
eccentricity 0.122
Perihelion - aphelion 37.961 AU - 48.51 AU
Inclination of the orbit plane 27.4 °
Length of the ascending node 78.3 °
Argument of the periapsis 224 °
Time of passage of the perihelion 4th August 1909
Sidereal period 284 a 3.5 M.
Mean orbital velocity 4.493 km / s
Physical Properties
Medium diameter 409 km
Albedo
Rotation period 7.92 ± 0.04 h (0.330 d )
Absolute brightness 4.5 - 4.81 ± 0.14 mag
Spectral class C
B-V = 0.670 ± 0.030
VR = 0.400 ± 0.020
VI = 0.750 ± 0.020
BR = 1.056 ± 0.210
history
Explorer Chadwick A. Trujillo ,
David C. Jewitt ,
Jane X. Luu
Date of discovery October 12, 1996
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.

(19308) 1996 TO 66 is a large trans-Neptunian object that is classified as an extended Scattered Disk Object (DO) or as a Cubewano (CKBO) and as a member of the Haumea family. Because of its size, the asteroid is a dwarf planet candidate .

discovery

1996 TO 66 was discovered on October 12, 1996 by a team of astronomers consisting of Chadwick A. Trujillo ( Gemini Observatory ), Dave Jewitt ( UCLA ) and Jane Luu ( Harvard ) with the 2.2 m UH telescope of the Mauna -Kea Observatory ( Hawaii ) discovered. The discovery was announced on June 18, 1997, the planetoid was later given the minor planet number 19308 by the IAU .

After its discovery, TO 66 could be identified in photos up to October 1, 1983, which were taken as part of the Digitized Sky Survey program (DSS) at the Siding Spring Observatory , in 1996 and thus extended its observation period by 13 years in order to calculate its orbit more precisely. In April 2017, a total of 177 observations were made over a period of 34 years. The last observation so far was carried out in October 2016 on the Pan-STARRS telescope (PS1). (As of March 7, 2019)

properties

Orbit

1996 TO 66 orbits the sun in 284.29 years on a slightly elliptical orbit between 37.96  AU and 48.51 AU from its center. The orbit eccentricity is 0.122, the orbit is 27.42 ° inclined to the ecliptic . The planetoid is currently 47.45 AU from the Sun. He passed through perihelion for the last time in 1909, so the next perihelion should take place in 2193.

Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center him as Cubewano classifies, where he ground dynamically to the "hot" classical KBO heard; the latter also lists it as a non-SDO and generally as a “distant object” . The asteroid is a member of the Haumea family, which consists of fragments from a previous collision on the dwarf planet Haumea .

Size and rotation

A diameter of 409 km is currently assumed, based on a reflectivity of 32.8% and an absolute brightness of 3.8  m . Assuming a diameter of 409 km, this results in a total surface of around 526,000 km². The apparent brightness of 1996 TO 66 is 21.58 m , the mean surface temperature is estimated at 45 K (−228 ° C) based on the distance from  the sun  .

Since it can be assumed that TO 66 could be in hydrostatic equilibrium due to its size and would therefore have to be largely round, it could meet the criteria for classification as a dwarf planet . Mike Brown , the self-km estimates the diameter of only 149, based on a higher albedo of 70% and an absolute magnitude of 5.2  m , assumes that it is at 1996 TO 66 to perhaps no concerns dwarf planet. Gonzalo Tancredi did not make a recommendation in 2010.

On the basis of light curve observations , TO 66 rotates once around its axis in 1996 in 7 hours and 55.2 minutes. This means that in a 1996 TO 66 year it performs 314661.8 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 1996 TO 66
year Dimensions km source
2004 <897.0 Altenhoff et al. a.
2005 <902.0 Grundy et al. a.
2010 529.0 Tancredi
2013 409.0 Mommert et al. a.
2015 574.81 LightCurve DataBase
2018 <330.0 Vilenius et al. a.
2018 149.0 Brown
The most precise determination is marked in bold .

See also

Web links

Individual evidence

  1. ^ Marc W. Buie : Orbit Fit and Astrometric record for 19308 . SwRI (Space Science Department). Retrieved March 7, 2019.
  2. ↑ a b MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 7, 2019.
  3. ^ A b Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 7, 2019.
  4. ↑ a b c (19308) 1996 TO66 at the IAU Minor Planet Center (English) Retrieved March 7, 2019.
  5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  6. ↑ a b c d M. Mommert u. a .: Remnant planetesimals and their collisional fragments: Physical characterization from thermal-infrared observations . September 23, 2013. Accessed March 4, 2019.
  7. ^ S. Sheppard , D. Jewitt : Hawaii Kuiper Belt Variability Project: An Update . In: Earth, Moon, and Planets . 92, No. 1, November 10, 2003, pp. 207-219. bibcode : 2003EM & P ... 92..207S . doi : 10.1023 / B: MOON.0000031943.12968.46 .
  8. ↑ a b E. Vilenius u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. XIV. Size / albedo characterization of the Haumea family observed with Herschel and Spitzer . In: Astronomy and Astrophysics . 618, no.A136, October 2018, p. 15. bibcode : 2018A & A ... 618A.136V . doi : 10.1051 / 0004-6361 / 201732564 .
  9. ↑ a b LCDB Data for (19308) 1996TO66 . MinorPlanetInfo. 2015. Accessed March 7, 2019.
  10. ↑ a b c I. Belskaya et al. a .: Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo . In: Icarus . 250, April 2015, pp. 482-491. bibcode : 2015Icar..250..482B . doi : 10.1016 / j.icarus.2014.12.004 .
  11. ↑ N. Peixinho et al. a .: The bimodal colors of Centaurs and small Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 546, No. A86, June 14, 2012, p. 12. arxiv : 1206.3153 . bibcode : 2012A & A ... 546A..86P . doi : 10.1051 / 0004-6361 / 201219057 .
  12. ↑ MPC : MPEC 1997-M05: 1996 TO66 . IAU . June 18, 1997. Retrieved March 7, 2019.
  13. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 7, 2019.
  14. ↑ (19308) 1996 TO66 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 7, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  15. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 7, 2019.
  16. ↑ (19308) 1996 TO66 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  17. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 7, 2019.
  18. ^ 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 7, 2019.
  19. ↑ W. Altenhoff u. a .: Size estimates of some optically bright KBOs (PDF) . In: Astronomy and Astrophysics . 415, Nov. 10, 2003, pp. 771-775. bibcode : 2004A & A ... 415..771A . doi : 10.1051 / 0004-6361: 20035603 .
  20. ↑ W. Grundy et al. a .: Various Albedos of Small Trans-Neptunian Objects (PDF) . In: Icarus . 176, No. 1, February 10, 2005, pp. 184-191. arxiv : astro-ph / 0502229 . bibcode : 2005Icar..176..184G . doi : 10.1016 / j.icarus.2005.01.007 .