(690420) 2014 FC72

Last updated

(690420) 2014 FC72
Discovery [1]
Discovered by Pan-STARRS 1
Discovery site Haleakala Obs.
Discovery date24 March 2014
(first observed only)
Designations
2014 FC72
Orbital characteristics [2]
Epoch 27 April 2019 (JD  2458600.5)
Uncertainty parameter 3
Observation arc 16.91  yr (6,178 d)
Aphelion 100.57  AU
Perihelion 51.663 AU
76.114 AU
Eccentricity 0.3212
664.06 yr (242,547 d)
357.23°
0° 0m 5.4s / day
Inclination 29.859°
178.00°
≈ 25 November 2023 [6]
±7 days
33.138°
Physical characteristics
Mean diameter
  • 0.08 (assumed) [7]
  • 0.09 (assumed) [5]
22.09 [8]
4.7 [1] [2]

    (690420) 2014 FC72 is a trans-Neptunian object, classified as a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 24 March 2014 by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. [1] With its perihelion distant from Neptune, it belongs to a small and poorly understood group of objects with moderate eccentricities. [9] [10] It is estimated to measure 500 kilometers (300 miles) in diameter, assuming a low albedo.

    Contents

    Orbit and classification

    The object is located in the "gap", a poorly understood region. Extreme transneptunian object eccentricity vs perihelion.png
    The object is located in the "gap", a poorly understood region.

    2014 FC72 orbits the Sun at a distance of 51.7–100.6  AU once every 664 years (242,547 days; semi-major axis of 76.11 AU). Its orbit has a moderate eccentricity of 0.32 and an inclination of 30° with respect to the ecliptic. [2]

    The object belongs to the same orbital group as 2004 XR190 ("Buffy"), 2014 FZ71 , 2015 FJ345 and 2015 KQ174 (also see diagram). With an orbital period of 664 years, they seem to be resonant trans-Neptunian objects in a 1:4 resonance with Neptune, as are 2003 LA7 and 2011 UP411, [5] but with lower eccentricities and therefore higher perihelia as the latter.

    Considered a scattered and detached object, [3] [4] [5] 2014 FC72 is particularly unusual as it has an unusually circular orbit for a scattered-disc object (SDO). Although it is thought that traditional scattered-disc objects have been ejected into their current orbits by gravitational interactions with Neptune, the low eccentricity of its orbit and the distance of its perihelion (SDOs generally have highly eccentric orbits and perihelia less than 38 AU) seems hard to reconcile with such celestial mechanics. This has led to some uncertainty as to the current theoretical understanding of the outer Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper belt, and resonance interaction with an outward-migrating Neptune. The Kozai mechanism is capable of transferring orbital eccentricity to a higher inclination. [10] [9]

    Physical characteristics

    2014 FC72 has a diameter estimated at around 500 kilometers (310 miles), roughly a fifth the size of Pluto. [5] [7]

    Related Research Articles

    A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has an orbital semi-major axis of 30.1 astronomical units (au).

    <span class="mw-page-title-main">Scattered disc</span> Collection of bodies in the extreme Solar System

    The scattered disc (or scattered disk) is a distant circumstellar disc in the Solar System that is sparsely populated by icy small Solar System bodies, which are a subset of the broader family of trans-Neptunian objects. The scattered-disc objects (SDOs) have orbital eccentricities ranging as high as 0.8, inclinations as high as 40°, and perihelia greater than 30 astronomical units (4.5×109 km; 2.8×109 mi). These extreme orbits are thought to be the result of gravitational "scattering" by the gas giants, and the objects continue to be subject to perturbation by the planet Neptune.

    <span class="nowrap">(612911) 2004 XR<sub>190</sub></span> Minor planet in the scattered disc

    (612911) 2004 XR190, nicknamed Buffy, is a trans-Neptunian object, classified as both a scattered disc object and a detached object, located in the outermost region of the Solar System. It was first observed on 11 December 2004, by astronomers with the Canada–France Ecliptic Plane Survey at the Mauna Kea Observatories, Hawaii, United States. It is the largest known highly inclined (> 45°) object. With a perihelion of 51 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities.

    (118228) 1996 TQ66 (provisional designation 1996 TQ66) is a resonant trans-Neptunian object of the plutino population in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 October 1996, by American astronomers Jun Chen, David Jewitt, Chad Trujillo, and Jane Luu, using the UH88 telescope at the Mauna Kea Observatories, Hawaii. The very red object measures approximately 185 kilometers (110 miles) in diameter. As of 2021, it has not been named.

    (35671) 1998 SN165 (provisional designation 1998 SN165) is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.

    <span class="nowrap">(40314) 1999 KR<sub>16</sub></span>

    (40314) 1999 KR16 is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 kilometers (158 miles) in diameter. It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESO's La Silla Observatory in northern Chile. The very reddish object is a dwarf planet candidate and has a rotation period of 11.7 hours.

    474640 Alicanto (provisional designation 2004 VN112) is a detached extreme trans-Neptunian object. It was discovered on 6 November 2004, by American astronomer Andrew C. Becker at Cerro Tololo Inter-American Observatory in Chile. It never gets closer than 47 AU from the Sun (near the outer edge of the main Kuiper belt) and averages more than 300 AU from the Sun. Its large eccentricity strongly suggests that it was gravitationally scattered onto its current orbit. Because it is, like all detached objects, outside the current gravitational influence of Neptune, how it came to have this orbit cannot yet be explained. It was named after Alicanto, a nocturnal bird in Chilean mythology.

    <span class="mw-page-title-main">Detached object</span> Dynamical class of minor planets

    Detached objects are a dynamical class of minor planets in the outer reaches of the Solar System and belong to the broader family of trans-Neptunian objects (TNOs). These objects have orbits whose points of closest approach to the Sun (perihelion) are sufficiently distant from the gravitational influence of Neptune that they are only moderately affected by Neptune and the other known planets: This makes them appear to be "detached" from the rest of the Solar System, except for their attraction to the Sun.

    (589683) 2010 RF43 (provisional designation 2010 RF43) is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observatory in northern Chile.

    <span class="mw-page-title-main">Sednoid</span> Group of Trans-Neptunian objects

    A sednoid is a trans-Neptunian object with a large semi-major axis and a high perihelion, similar to the orbit of Sedna. The consensus among astronomers is that there are only three objects that are known from this population: 90377 Sedna, 2012 VP113, and 541132 Leleākūhonua (2015 TG387). All three have perihelia greater than 60 AU. These objects lie outside an apparently nearly empty gap in the Solar System and have no significant interaction with the planets. They are usually grouped with the detached objects. Some astronomers consider the sednoids to be Inner Oort Cloud (IOC) objects, though the inner Oort cloud, or Hills cloud, was originally predicted to lie beyond 2,000 AU, beyond the aphelia of the three known sednoids.

    2003 SS422 is a trans-Neptunian object located in the outermost region of the Solar System. It was discovered on 28 September 2003, by American astronomers at the Cerro Tololo Observatory in La Serena, Chile, and estimated to measure approximately 168 kilometers (104 miles) in diameter.

    (533560) 2014 JM80 (provisional designation 2014 JM80) is a trans-Neptunian object (TNO) from the scattered disc in the outermost Solar System, approximately 340 kilometers (210 miles) in diameter. It was discovered on 9 May 2010 by astronomers with the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael Brown, it is "possibly" a dwarf planet.

    2014 FZ71 is a trans-Neptunian object, a scattered disc classified as a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 24 March 2014, by a team led by American astronomer Scott Sheppard at the Cerro Tololo Inter-American Observatory in Chile. With its perihelion of almost 56 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities. The object is not a dwarf planet candidate as it only measures approximately 150 kilometers (93 miles) in diameter.

    2015 FJ345 is a trans-Neptunian object and detached object, located in the scattered disc, the outermost region of the Solar System. It was first observed on 17 March 2015, by a team led by American astronomer Scott Sheppard at the Mauna Kea Observatories, in Hawaii, United States. With its perihelion of almost 51 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities. The object is not a dwarf planet candidate as it only measures approximately 120 kilometers (75 miles) in diameter.

    2015 KQ174 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. The object with a moderately inclined and eccentric orbit measures approximately 154 kilometers (96 miles) in diameter. It was first observed on 24 May 2015, by astronomers at the Mauna Kea Observatories in Hawaii, United States.

    (523635) 2010 DN93 (provisional designation 2010 DN93) is a trans-Neptunian object from in the scattered disc located in the outermost region of the Solar System. It was discovered on 26 February 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. Assuming a low albedo, the object is estimated at approximately 490 kilometers (300 miles) in diameter. It was numbered in 2018 and remains unnamed.

    <span class="nowrap">2013 FQ<sub>28</sub></span>

    2013 FQ28 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 17 March 2013, by a team of astronomers at the Cerro Tololo Inter-American Observatory in Chile. It orbits the Sun in a moderate inclined, moderate-eccentricity orbit. The weak dwarf planet candidate measures approximately 260 kilometers (160 miles) in diameter.

    2013 SK100 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. The object with a moderately inclined and eccentric orbit measures approximately 135 kilometers (84 miles) in diameter. It was first observed on 29 September 2013, by astronomers at the Mauna Kea Observatories in Hawaii, United States.

    2014 ST373 (prov. designation:2014 ST373) is a trans-Neptunian object and a detached object from the outermost region of the Solar System. With a perihelion of 50.2 AU, it belongs to the top 10 minor planets with the highest known perihelia of the Solar System. and is neither a scattered disc nor an extreme trans-Neptunian object. It measures approximately 370 kilometers (230 miles) in diameter and was first observed on 25 September 2014, by astronomers using the Dark Energy Camera (DECam) at Cerro Tololo Inter-American Observatory in Chile.

    References

    1. 1 2 3 4 "2014 FC72". Minor Planet Center. Retrieved 12 December 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: (2014 FC72)" (2017-04-03 last obs.). Jet Propulsion Laboratory . Retrieved 12 December 2018.
    3. 1 2 Jewitt, David, Morbidelli, Alessandro, & Rauer, Heike. (2007). Trans-Neptunian Objects and Comets: Saas-Fee Advanced Course 35. Swiss Society for Astrophysics and Astronomy. Berlin: Springer. ISBN   3-540-71957-1.
    4. 1 2 Lykawka, Patryk Sofia; Mukai, Tadashi (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus. 189 (1): 213–232. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001.
    5. 1 2 3 4 5 6 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 12 December 2018.
    6. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    7. 1 2 3 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 12 December 2018.
    8. ↑ "2014 FC72 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site, Department of Mathematics, University of Pisa, Italy. Retrieved 12 December 2018.
    9. 1 2 Sheppard, Scott S.; Trujillo, Chadwick; Tholen, David J. (July 2016). "Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects with Moderate Semimajor Axes and Eccentricities". The Astrophysical Journal Letters. 825 (1): 7. arXiv: 1606.02294 . Bibcode:2016ApJ...825L..13S. doi: 10.3847/2041-8205/825/1/L13 . S2CID   118630570.
    10. 1 2 Allen, R. L.; Gladman, B.; Kavelaars, J. J.; Petit, J.-M.; Parker, J. W.; Nicholson, P. (March 2006). "Discovery of a Low-Eccentricity, High-Inclination Kuiper Belt Object at 58 AU". The Astrophysical Journal. 640 (1): L83–L86. arXiv: astro-ph/0512430 . Bibcode:2006ApJ...640L..83A. doi:10.1086/503098. S2CID   15588453. (Discovery paper)
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