(469615) 2004 PT 107

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Asteroid
(469615) 2004 PT 107
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type CKBO  ( «Hot» )  or
DO (E SDO ),
«Distant Object»
Major semi-axis 40.679  AU
eccentricity 0.061
Perihelion - aphelion 38.213 AU - 43.145 AU
Inclination of the orbit plane 26.1 °
Length of the ascending node 320.9 °
Argument of the periapsis 17 °
Time of passage of the perihelion June 1, 2019
Sidereal period 259 a 5.5 M
Mean orbital velocity 4.632 km / s
Physical Properties
Medium diameter
Albedo
Rotation period 20 h (0.833 d )
Absolute brightness 6.33 ± 0.11 mag
Spectral class C.
history
Explorer Marc W. Buie
Lawrence H. Wasserman
David E. Trilling
J.R. Lovering
James L. Elliot
JF Kane
M. E. Teyssier
Robert L. Millis
Date of discovery August 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.

(469615) 2004 PT 107 is a large trans-Neptunian object in the Kuiper belt , which is classified as a Cubewano (CKBO) or an extended Scattered Disk Object (DO) in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2004 PT 107 was won on August 13, 2004 by Marc Buie (official) as well as Larry Wasserman, David Trilling, J. Lovering, James Elliot , J. Kane, M. Teyssier and Robert Millis with the 4.0 – m – Víctor M. Blanco telescope (DECam) discovered at Cerro Tololo Observatory ( Chile ). The discovery was announced on September 4, 2004 together with 2003 QF 113 , 2004 OJ 14 , 2004 PR 107 and 2004 PS 107 , the planetoid was later given the minor planet number 469615 by the IAU .

The asteroid's observation sheet begins with the official discovery observation on August 13, 2004. In April 2017, a total of 153 observations were made over a period of 11 years. The last observation so far was carried out in July 2015 on the Pan-STARRS telescope (PS1). (As of March 8, 2019)

properties

Orbit

2004 PT 107 orbits the sun in 259.46 years on a slightly elliptical orbit between 38.21  AU and 43.14 AU from its center. The orbit eccentricity is 0.061, the orbit is 26.08 ° inclined to the ecliptic . Currently, the planetoid is 38.22 AU from the sun. The last time he passed through perihelion in 2019, the next perihelion should therefore take place in 2278.

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” .

Size and rotation

A diameter of 400 km is currently assumed, based on a reflectivity of 3.2% and an absolute brightness of 6.33  m . Based on this diameter, the total surface area is around 503,000 km 2 . The apparent magnitude of 2004 PT 107 is 22.02  m .

Since it is conceivable that 2004 PT 107 is in hydrostatic equilibrium due to its size and could thus be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown , who estimates the diameter to be only 290 km ( albedo 8%, absolute brightness 6.1  m ), assumes that 2004 PT 107 is just perhaps a dwarf planet.

Using light curve observations , 2004 PT 107 rotates once around its axis every 20 hours. From this it follows that in a 2004 PT 107 year it performs 113 719.7 self- rotations (“days”). However, since the observation time at that time was not sufficient, this result is inconclusive.

Provisions of the diameter for 2004 PT 107
year Dimensions km source
2012 290.75 LightCurve DataBase
2014 330.0 +110.0−100.0 Lellouch u. a.
2014 400.0 +45.0−51.0 Vilenius et al. a.
2018 290.0 Brown
The most precise determination is marked in bold .

See also

Web links

Individual evidence

  1. ↑ a b MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 8, 2019.
  2. ↑ a b E. Lellouch u. a .: "TNOs are Cool": A survey of the trans-Neptunian region. IX. Thermal properties of Kuiper belt objects and Centaurs from combined Herschel and Spitzer observations (PDF) . In: Astronomy and Astrophysics . 557, No. A60, June 10, 2013, p. 19. bibcode : 2013A & A ... 557A..60L . doi : 10.1051 / 0004-6361 / 201322047 .
  3. ^ A b Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 8, 2019.
  4. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 469615 . SwRI (Space Science Department). Retrieved March 8, 2019.
  5. ↑ a b c (469615) 2004 PT107 at the IAU Minor Planet Center (English) Retrieved March 8, 2019.
  6. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  7. ↑ a b c d E. Vilenius u. a .: “TNOs are cool”: A survey of the trans-Neptunian region X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations (PDF) . In: Astronomy and Astrophysics . 564, No. A35, March 25, 2014, p. 18. arxiv : 1403.6309 . doi : 10.1051 / 0004-6361 / 201322416 .
  8. ↑ C. Snodgrass et al. a .: Characterization of candidate members of (136108) Haumea's family . In: EDP Sciences (Ed.): Astronomy and Astrophysics . 511, December 16, 2009, p. A72. arxiv : 0912.3171 . bibcode : 2010A & A ... 511A..72S . doi : 10.1051 / 0004-6361 / 200913031 .
  9. ↑ a b LCDB Data for (469615) 2004PT107 . MinorPlanetInfo. 2012. Retrieved March 8, 2019.
  10. ^ MPC : List Of Transneptunian Objects . IAU . Retrieved March 8, 2019.
  11. ↑ MPC : MPEC 2004-R15: 2003 QF113, 2004 OJ14, 2004 PR107, 2004 PS107, 2004 PT107 . IAU . September 4, 2004. Retrieved March 8, 2019.
  12. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 8, 2019.
  13. ↑ (469615) 2004 PT107 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 8, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  14. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 8, 2019.
  15. ↑ (469615) 2004 PT107 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  16. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 8, 2019.