(175113) 2004 PF 115

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Asteroid
(175113) 2004 PF 115
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type CKBO ( "Hot" ),
"Distant Object"
Major semi-axis 39,068  AU
eccentricity 0.065
Perihelion - aphelion 36.518 AU - 41.619 AU
Inclination of the orbit plane 13.3 °
Length of the ascending node 84.4 °
Argument of the periapsis 87.2 °
Time of passage of the perihelion December 1, 1905
Sidereal period 244 a 2.4 M
Mean orbital velocity 4.726 km / s
Physical Properties
Medium diameter
Albedo
Absolute brightness 4.3 - 4.54 ± 0.25 mag
history
Explorer Michael E. Brown
Chadwick A. Trujillo
David L. Rabinowitz
Date of discovery August 7, 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.

(175113) 2004 PF 115 is a large trans-Neptunian object in the Kuiper belt , which is classified as Cubewano in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2004 PF 115 was discovered on August 7, 2004 by a team of astronomers consisting of Mike Brown , Chad Trujillo and David Lincoln Rabinowitz as part of the Near Earth Asteroid Tracking Project (NEAT) with the 1.2 m Oschin Schmidt telescope discovered at Palomar Observatory, California . The discovery was made with 2004 XA 192 , 2005 QU 182 and 2004 PG 115 announced on 1 September 2007, the asteroid was on 20 January 2008 by the IAU , the minor planet number one hundred and seventy-five thousand one hundred thirteen .

After its discovery, in 2004 PF 115 could be identified in photos taken as part of the Digitized Sky Survey program at the Siding Spring Observatory ( Australia ) up to June 4, 1992, thus extending its observation period by 12 years in order to calculate its orbit more precisely. Since then, the planetoid has been observed with the Herschel space telescope as well as earth-based telescopes. In April 2017, a total of 124 observations were made over a period of 24 years. The last observation so far was carried out in September 2018 at the Purple Mountain Observatory ( People's Republic of China ). (As of February 25, 2019)

properties

Orbit

2004 PF 115 orbits the sun in 244.20 years on a slightly elliptical orbit between 36.52  AU and 41.62 AU from its center. The orbit eccentricity is 0.065, the orbit is inclined 13.35 ° to the ecliptic . The planetoid is currently 41.56 AU from the Sun. He passed perihelion for the last time in 1905, so the next perihelion is likely to take place in 2150.

Marc Buie ( DES ) classifies the planetoid as Cubewano , whereby it belongs to the orbital dynamics “hot” classical KBO , while the Minor Planet Center classifies it as a non-SDO and generally as a “distant object” .

Size and rotation

A diameter of around 468 km is currently assumed, based on a reflectivity of 12.3% and an absolute brightness of 4.54  m , which was determined by the Herschel space telescope. Assuming a diameter of 468.2 km, this results in a total surface area of ​​around 689,000 km 2 . The apparent brightness of 2004 PF 115 is 20.86  m , the mean surface temperature is estimated at 44 K (−229 ° C) based on the distance from the sun  .

Since it can be assumed that 2004 PF 115 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 expects that it is at 2004 PF 115 to possibly is a dwarf planet. Gonzalo Tancredi did not make a recommendation in 2010.

Provisions of the diameter for 2004 PF 115
year Dimensions km source
2010 482.0 Tancredi
2012 406.3 +97.6-75.3
468.2 +38.6−49.1 		Mommert et al. a.
2018 482.0 Brown
The most precise determination is marked in bold .

See also

Web links

Individual evidence

  1. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 175113 . SwRI (Space Science Department). Retrieved February 25, 2019.
  2. ↑ a b c (175113) 2004 PF115 at the IAU Minor Planet Center (English) Retrieved February 25, 2019.
  3. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  4. ↑ a b c d M. Mommert u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. V. Physical characterization of 18 Plutinos using Herschel-PACS observations . In: Astronomy and Astrophysics . 541, no.A93 , February 16, 2012. arxiv : 1202.3657 . bibcode : 2012A & A ... 541A..93M . doi : 10.1051 / 0004-6361 / 201118562 .
  5. ↑ MPC : MPEC 2007-R03: 2004 PF115, 2004 PG115, 2004 XA192, 2005 QU182 . IAU . September 1, 2007. Retrieved February 25, 2019.
  6. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved February 25, 2019, reference there: MPC 61726
  7. ↑ (175113) 2004 PF115 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved February 25, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  8. ^ Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved February 25, 2019.
  9. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved February 25, 2019.
  10. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved February 25, 2019.
  11. ↑ (175113) 2004 PF115 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  12. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved February 25, 2019.
  13. ↑ a b Gonzalo 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 February 25, 2019.