2014 FC ₇₂

Asteroid 2014 FC 72
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	DO (E SDO ) or SDO , "Distant Object"
Major semi-axis	76.114  AU
eccentricity	0.321
Perihelion - aphelion	51.662 AU - 100.566 AU
Inclination of the orbit plane	29.9 °
Length of the ascending node	178 °
Argument of the periapsis	29.9 °
Time of passage of the perihelion	June 5, 2024
Sidereal period	664 a 0.7 M.
Mean orbital velocity	3.386 km / s
Physical Properties
Medium diameter	${\displaystyle 450_{-50}^{+50}\mathrm {km} }$
Albedo	0.08-0.09
Absolute brightness	4.7 - 4.9 mag
history
Explorer	Pan-STARRS : B. Gibson T. Goggia N. Primak A. Schultz M. Willman
Date of discovery	March 24, 2014
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.

2014 FC ₇₂ is a large trans-Neptunian object that is classified as a near or extended Scattered Disc Object (SDO or DO) in terms of orbit dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2014 FC ₇₂ was discovered on March 24, 2014 by a team of astronomers consisting of B. Gibson, T. Goggia, N. Primak, A. Schultz and M. Willman as part of the Pan-STARRS project with the 1.8 m –Ritchey-Chretien – Telescope (PS1) discovered at Haleakalā Observatory ( Maui ). The discovery was announced on July 17, 2016.

After its discovery, in 2014 FC _{72 could be identified} on photos taken as part of the Sloan Digital Sky Survey program at the Apache Point Observatory ( New Mexico ) up to May 4, 2000, thus changing its observation period Extend 12 years to more accurately calculate its orbit. In September 2018, a total of 122 observations were made over a period of 17 years. The last observation so far was again carried out in April 2017 at the Pan-STARRS telescope. (As of March 3, 2019)

properties

2014 FC ₇₂ in the so-called “gap”.

Orbit

2014 FC ₇₂ orbits the sun in 664.06 years on a highly elliptical orbit between 34.35  AU and 266.14 AU from its center. The orbital eccentricity is 0.321, the orbit is 29.85 ° inclined to the ecliptic . The planetoid is currently 51.73 AU from the sun. He will next pass perihelion in 2024, so the last perihelion should have occurred in 1360.

2014 FC ₇₂ belongs to the same small group of detached objects as 2004 XR ₁₉₀ , 2014 FZ ₇₁ , 2015 FJ _345, and 2015 KQ ₁₇₄ , all of which have poorly understood orbits with large perihelia and moderate eccentricities. The asteroid moves beyond the Kuiper belt around the sun, possibly based on the orbital period of 664 years there is a 1: 4 orbital resonance to Neptune , as in 2003 LA ₇ and 2011 UP ₄₁₁ , but with lower eccentricity and consequently a higher perihelion than that the latter.

2014 FC ₇₂ is unusual in that it has an unusually circular orbit for an SDO. Although it is believed that ordinary SDOs got into their current orbit through interactions with Neptune, the low eccentricity and perihelion (SDOs generally have highly eccentric orbits and perihelia below 38 AU) have led to difficulties with the theoretical understanding of the celestial mechanics of the outer solar system. These theories include nearby passages of stars, unknown planets / protoplanets / solitary planets in the early Kuiper Belt, and orbital disturbances due to resonance effects with an outward migrating Neptune. The Kozai effect can convert orbit eccentricity into a higher orbit inclination.

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 it as an SDO.

size

A diameter of around 450 km is currently assumed; However, this is still fraught with some uncertainty. Assuming a diameter of 450 km, this results in a total surface of around 636,000 km ² . The apparent magnitude of 2014 FC ₇₂ is 22.03  ^m .

Since it can be assumed that 2014 FC ₇₂ 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 2014 FC ₇₂ is likely a dwarf planet. The latter estimates the diameter at 513 km, based on a reflectivity of 8% and an absolute brightness of 4.9  ^m .

Provisions of the diameter for 2014 FC ₇₂

year	Dimensions km	source
2016	450.0 ± 50.0	Sheppard et al. a.
2018	509.0	Johnston
2018	513.0	Brown
The most precise determination is marked in bold .

Trans-Neptunian objects on the edge of the Kuiper belt with perihelia q> 47 AU

object	q (AU)	a (AU)	T ( a )	e	i (°)	ω (°)	H (likes)
2012 VP 113	80.39	258.27	4.151	0.69	24.1	293.5	4.0
(90377) Sedna	76.26	484.52	10,665	0.84	11.9	311.4	1.3
(541132) Leleākūhonua	65.04	1031.49	33,128	0.94	11.7	118.0	5.5
2014 FZ 71	55.88	75.76	659	0.26	25.5	244.5	6.9
2015 RG 301	52.05	54.04	397	0.04	10.2	287.4	8.2
2014 FC 72	51.66	75.75	659	0.32	29.9	33.3	4.7
2018 GT 15	51.54	57.58	437	0.10	26.0	357.3	7.5
2004 XR 190	51.11	57.26	433	0.11	46.8	285.6	4.3
2015 FJ 345	50.69	62.88	499	0.19	35.0	77.4	7.9
2014 ST 373	50.19	104.56	1,069	0.52	43.2	297.1	5.4
2013 SY 99	50.02	693.86	18,277	0.93	4.2	32.1	6.7
2015 KQ 174	49.31	55.40	412	0.11	24.3	294.0	7.3
2010 GB 174	48.75	350.59	6,565	0.86	21.6	347.4	6.5
2014 SR 349	47.69	302.23	5,254	0.84	18.0	340.9	6.7
(474640) 2004 VN 112	47.30	318.97	5,697	0.85	25.6	326.8	6.5

See also

• List of trans-Neptunian objects
• List of dwarf planets of the solar system
• List of asteroids
• List of moons from asteroids

Web links

• How many dwarf planets are there in the outer solar system? Current list of the largest TNOs from Mike Brown
• Free the dwarf planets! Mike Brown's column on the IAU and the dwarf planets regarding their classifications (23 August 2011)

Individual evidence

1. ^ ^{A b} Marc W. Buie : Orbit Fit and Astrometric record for 14FC72 . SwRI (Space Science Department). Retrieved March 3, 2019.
2. ↑ P. Lykawka et al. a .: Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects With Moderate Semi-major Axes and Eccentricities . In: Icarus . 189, No. 1, July 2007, pp. 213-232. bibcode : 2007Icar..189..213L . doi : 10.1016 / j.icarus.2007.01.001 .
3. ↑ ^{a b c} Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 3, 2019.
4. ↑ ^{a b c} 2014 FC72 at the IAU Minor Planet Center (English) Retrieved March 3, 2019.
5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
6. ↑ ^{a b} S. Sheppard et al. a .: Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects With Moderate Semi-major Axes and Eccentricities (PDF) . In: The Astronomical Journal Letters . 825, No. 1, June 7, 2016, p. L13, 7. arxiv : 1606.02294 . bibcode : 2016ApJ ... 825L..13S . doi : 10.3847 / 2041-8205 / 825/1 / L13 .
7. ↑ MPC : MPEC 2016-0197: 2014 FC72 . IAU . July 17, 2016. Retrieved March 3, 2019.
8. ↑ 2014 FC72 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 3, 2019.
9. ↑ R. Allen et al. a .: Discovery of a Low-Eccentricity, High-Inclination Kuiper Belt Object at 58 AU (PDF) . In: The Astronomical Journal . 640, No. 1, December 16, 2005, pp. L83-L86. arxiv : astro-ph / 0512430 . bibcode : 2006ApJ ... 640L..83A . doi : 10.1086 / 503098 .
10. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 3, 2019.
11. ↑ 2014 FC72 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 March 3, 2019.
13. ↑ List of objects with q> 47. Minor Planet Center (MPC) of the International Astronomical Union (IAU), accessed on June 13, 2020 . 
14. ↑ Chadwick A. Trujillo, Michael E. Brown: The Radial Distribution of the Kuiper Belt . In: The Astrophysical Journal Letters . Vol. 554, No. 1 , May 31, 2001, p. L95 , doi : 10.1086 / 320917 , bibcode : 2001ApJ ... 554L..95T (English).