2014 FZ71

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2014 FZ71
Discovery [1]
Discovered by CTIO
Discovery site CTIO
(first observed only)
Discovery date24 March 2014
Designations
2014 FZ71
Orbital characteristics [2]
Epoch 27 April 2019 (JD  2458600.5)
Uncertainty parameter 6
Observation arc 1.96  yr (716 d)
Aphelion 95.791  AU
Perihelion 55.849 AU
75.820 AU
Eccentricity 0.2634
660.21 yr (241,142 d)
349.80°
0° 0m 5.4s / day
Inclination 25.506°
306.01°
244.94°
Physical characteristics
Mean diameter
  • 0.08 (assumed) [7]
  • 0.09 (assumed) [5]
24.61 [8]
6.9 [1] [2]

    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. [6] [9] The object is not a dwarf planet candidate as it only measures approximately 150 kilometers (93 miles) in diameter.

    Contents

    Discovery and naming

    2014 FZ71 was first observed on 24 March 2014 by a team of astronomers led by Scott Sheppard of the Carnegie Institution for Science as part of the survey for distant solar system objects beyond the Kuiper Cliff using the new wide-field cameras on the Subaru and Cerro Tololo Inter-American Observatory (CTIO) telescopes. [6]

    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 FZ71 orbits the Sun at a distance of 55.8–95.8  AU once every 660 years and 3 months (241,142 days; semi-major axis of 75.82 AU). Its orbit has a moderate eccentricity of 0.26 and an inclination of 26° with respect to the ecliptic. [2]

    The object belongs to the same orbital group as 2004 XR190 ("Buffy"), 2014 FC72 , 2015 FJ345 and 2015 KQ174 (also see diagram). With an orbital period of 660 years, it seems to be resonant trans-Neptunian objects in a 1:4 resonance with Neptune, as are 2003 LA7 and 2011 UP411, [5] but with a lower eccentricity and therefore higher perihelion.

    Considered a scattered and detached object, [3] [4] [5] 2014 FZ71 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. [9]

    Physical characteristics

    2014 FZ71 has a diameter estimated between 125 and 185 kilometers, [6] [7] [5] roughly a quarter the size of 2004 XR190 ("Buffy") which is estimated at 500 kilometres (310 mi), roughly a quarter the size of Pluto. It is therefore not a dwarf planet candidate. [7]

    Related Research Articles

    <span class="mw-page-title-main">Trans-Neptunian object</span> Solar system objects beyond Neptune

    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.

    (119070) 2001 KP77, provisional designation:2001 KP77, is a resonant trans-Neptunian object in the Kuiper belt, a circumstellar disc located in the outermost region of the Solar System. It was discovered on 23 May 2001, by American astronomer Marc Buie at the Cerro Tololo Observatory in Chile. The object is locked in a 4:7 orbital resonance with Neptune. It has a red surface color and measures approximately 176 kilometers (110 miles) in diameter. As of 2021, it has not been named.

    <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.

    <span class="nowrap">2012 VP<sub>113</sub></span> Trans-Neptunian object

    2012 VP113, also known by its nickname "Biden", is a trans-Neptunian object of the sednoid population, located in the outermost reaches of the Solar System. It was first observed on 5 November 2012 by American astronomers Scott Sheppard and Chad Trujillo at the Cerro Tololo Inter-American Observatory in Chile. The discovery was announced on 26 March 2014. The object probably measures somewhere between 300 and 1000 km in diameter, possibly large enough to be a dwarf planet.

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

    A sednoid is a trans-Neptunian object with a perihelion well beyond the Kuiper cliff at 47.8 AU. Only four objects are known from this population: 90377 Sedna, 2012 VP113, 541132 Leleākūhonua (2015 TG387), and 2021 RR205, but it is suspected that there are many more. All four have perihelia greater than 55 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 objects (OCOs), though the inner Oort cloud, or Hills cloud, was originally predicted to lie beyond 2,000 AU, beyond the aphelia of the four known sednoids.

    <span class="nowrap">2014 FC<sub>69</sub></span>

    2014 FC69 is a trans-Neptunian object of the scattered disc on an eccentric orbit in the outermost region of the Solar System. It was first observed on 25 March 2014, by American astronomers Scott Sheppard and Chad Trujillo at the Cerro Tololo Observatory in Chile. It is one of the most distant objects from the Sun, even further away than Sedna.

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

    2013 FS28 is an extreme trans-Neptunian object from the extended scattered disc on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 466 kilometers (290 miles) in diameter. The detached, extended scattered disc object belongs to the group of extreme trans-Neptunian objects. It was first observed on 16 March 2013, by American astronomers Scott Sheppard and Chad Trujillo at the Cerro Tololo Observatory in Chile.

    (533560) 2014 JM80, provisional designation 2014 JM80, is a trans-Neptunian object 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.

    <span class="nowrap">2015 BP<sub>519</sub></span> Extreme trans-Neptunian object

    2015 BP519, nicknamed Caju, is an extreme trans-Neptunian object from the scattered disc on a highly eccentric and inclined orbit in the outermost region of the Solar System. It was first observed on 17 January 2015, by astronomers with the Dark Energy Survey at Cerro Tololo Observatory (W84) in Chile. It has been described as an extended scattered disc object (ESDO), and fits into the group of extreme objects that led to the prediction of Planet Nine, and has the highest orbital inclination of any of these objects.

    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. With its perihelion distant from Neptune, it belongs to a small and poorly understood group of objects with moderate eccentricities. It is estimated to measure 500 kilometers (300 miles) in diameter, assuming a low albedo.

    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.

    <span class="nowrap">2014 SV<sub>349</sub></span>

    2014 SV349 is a large trans-Neptunian object from the scattered disc located in the outermost region of the Solar System. It is one of the most distant objects from the Sun at 60.5 AU. The object is a dwarf planet candidate and measures approximately 423 kilometers (260 miles) in diameter. It was discovered on 19 September 2014, by American astronomer Scott Sheppard at the Cerro Tololo Observatory, Chile, and was provisionally designated 2014 SV349.

    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 "2014 FZ71". Minor Planet Center. Retrieved 12 December 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: (2014 FZ71)" (2016-03-09 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. 1 2 3 4 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.
    7. 1 2 3 4 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 12 December 2018.
    8. ↑ "2014 FZ71 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site, Department of Mathematics, University of Pisa, Italy. Retrieved 12 December 2018.
    9. 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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