2014 FE72

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2014 FE72
2014 FE72-orbit.png
Diagram showing the highly eccentric orbit of 2014 FE72
Discovery [1]
Discovered by
Discovery site Cerro Tololo Obs.
Discovery date26 March 2014
Designations
2014 FE72
Orbital characteristics [2]
Epoch 21 January 2022 (JD  2459600.5)
Uncertainty parameter 3
Observation arc 6.98 yr (2,549 days)
Aphelion
  • 4052 AU (barycentric) [3]
Perihelion
  • 36.101 AU (barycentric) [3]
  • 2045 AU (barycentric) [3]
Eccentricity
  • 0.9823 (barycentric) [3]
  • 92400 yr (barycentric) [3]
  • 0.219° (barycentric) [3]
0° 0m 0.055s / day
Inclination
  • 20.633° (barycentric) [3]
  • 336.829° (barycentric) [3]
≈ 6 October 1965 [4]
±11 days
  • 133.921° (barycentric) [3]
Physical characteristics
Mean diameter
270  km (est. at 0.08) [5] [6]
24.3 [7]
6.19 [2]

    2014 FE72 is a trans-Neptunian object first observed on 26 March 2014, at Cerro Tololo Inter-American Observatory in La Serena, Chile. It is a possible dwarf planet, [5] a member of the scattered disc, whose orbit extends into the inner Oort cloud. [1] Discovered by Scott Sheppard and Chad Trujillo, the object's existence was revealed on 29 August 2016. [1] [8] Both the orbital period and aphelion distance of this object are well constrained. [2] 2014 FE72 had the largest barycentric aphelion until 2018. However, the heliocentric aphelion of 2014 FE72 is second among trans-Neptunian objects (after the damocloid 2017 MB7 ). As of 2023, it is about 66 AU (9.9  billion   km ) from the Sun. [7]

    Contents

    Orbit

    Using the Solar System Barycenter as the orbital frame of reference, 2014 FE72's extremely elongated orbit (eccentricity = 0.98) has a perihelion of 36.1  AU, an aphelion of ~4,050 AU and a barycentric orbital period of ~92,400 years. [3] The latter values are the largest known for any Solar System body that is not a long-period comet. [n 1] Based on the barycentric orbital period, 2014 FE72 takes roughly 5 times longer than Sedna to orbit the Sun. [10]

    2014 FE72 last passed through perihelion around late 1965. [2]

    See also

    Notes

    1. ↑ 2017 MB7, an apparently much smaller object (absolute magnitude ~14) which might be an extinct comet, has a similar barycentric aphelion of ~2,800 AU and an orbital period of ~54,000 years. [9]

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    References

    1. 1 2 3 Williams, G. V. (29 August 2016). "MPEC 2016-Q43 : 2014 FE72". Minor Planet Center . Retrieved 31 August 2016.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: (2014 FE72)" (2021-03-18 last obs). Jet Propulsion Lab. Archived from the original on 5 February 2018. Retrieved 26 August 2018.
    3. 1 2 3 4 5 6 7 8 9 10 Horizons. "JPL Horizons: Barycentric Osculating Orbital Elements for 2014 FE72" . Retrieved 6 June 2022.
    4. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    5. 1 2 Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology . Retrieved 15 September 2016.
    6. ↑ "Absolute magnitude (H)". Near Earth Object Program. NASA/Jet Propulsion Lab. Archived from the original on 2 March 2001. Retrieved 15 September 2016.
    7. 1 2 "AstDyS 2014FE72 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 31 October 2023. (Distance to Sun [R] from 2023 to 2028.)
    8. ↑ "Hunt for ninth planet reveals new extremely distant Solar System objects". CarnegieScience.edu. Carnegie Institution. 29 August 2016. Retrieved 31 August 2016.
    9. ↑ JPL Small-Body Database Browser: (2017 MB7)
    10. ↑ Horizons. "JPL Horizons: Barycentric Osculating Orbital Elements for (90377) Sedna" . Retrieved 12 November 2018.
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