(533560) 2014 JM80

Last updated

(533560) 2014 JM80
Discovery [1]
Discovered by Pan-STARRS 1
Discovery site Haleakala Obs.
Discovery date9 May 2010
Designations
(533560) 2014 JM80
2014 JM80
TNO [2]  · SDO [3] [4]
distant [1]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc 2.93 yr (1,070 d)
Aphelion 80.184 AU
Perihelion 45.965 AU
63.074 AU
Eccentricity 0.2713
500.94 yr (182,969 d)
343.18°
0° 0m 7.2s / day
Inclination 20.479°
182.43°
≈ 20 November 2042 [5]
±8 days
96.342°
Physical characteristics
Mean diameter
329  km [6]
352 km [3]
5.5 [1] [2]

    (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. [1] According to American astronomer Michael Brown, it is "possibly" a dwarf planet. [3] [6]

    Contents

    Orbit and classification

    2014 JM80 is located near the TNO "gap", a poorly understood region. Extreme transneptunian object eccentricity vs perihelion.png
    2014 JM80 is located near the TNO "gap", a poorly understood region.

    2014 JM80 orbits the Sun at a distance of 46.0–80.2  AU once every 500 years and 11 months (182,969 days; semi-major axis of 63.07 AU). Its orbit has an eccentricity of 0.27 and an inclination of 20° with respect to the ecliptic. [2]

    This distant minor planet is a trans-Neptunian object and a member of the scattered disc population. Scattered-disc objects are thought to have been ejected from the classical Kuiper belt into their current orbits by gravitational interactions with Neptune, and typically have highly eccentric orbits and perihelia of less than 38 AU.

    2014 JM80 has also been considered a detached object, [7] [8] since its relatively low eccentricity of 0.27, and its perihelion distance of 46.0 AU are hard to reconcile with the celestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost 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] [10]

    With an orbital period of 500 years, and similar to 2015 FJ345 , it seems to be a resonant trans-Neptunian objects in a 1:3 resonance with Neptune, [9] : 12  as several other objects, but with a lower eccentricity (0.27 instead of more than 0.60) and a higher perihelia (at 45.8 AU rather than 31–41 AU). 2014 JM80 seems to belong to the same group as 2005 TB190 .[ citation needed ]

    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.

    <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">(612584) 2003 QX<sub>113</sub></span>

    (612584) 2003 QX113 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. It was discovered by astronomers with the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories, Hawaii, when it was near aphelion on 31 August 2003. It was provisionally designated 2003 QX113.

    (307463) 2002 VU130 (provisional designation 2002 VU130) is a trans-Neptunian object, located in the circumstellar disc of the Kuiper belt in the outermost region of the Solar System. The resonant trans-Neptunian object belongs to the population of plutinos and measures approximately 253 kilometers (160 miles) in diameter. It was discovered on 7 November 2002, by American astronomer Marc Buie at the Kitt Peak Observatory near Tucson, Arizona. The object has not been named yet.

    (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.

    (445473) 2010 VZ98 (provisional designation 2010 VZ98) is a trans-Neptunian object of the scattered disc, orbiting the Sun in the outermost region of the Solar System. It has a diameter of approximately 400 kilometers.

    <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. 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 objects (OCOs), 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.

    <span class="mw-page-title-main">Extreme trans-Neptunian object</span> Solar system objects beyond the other known trans-Neptunian objects

    An extreme trans-Neptunian object (ETNO) is a trans-Neptunian object orbiting the Sun well beyond Neptune (30 AU) in the outermost region of the Solar System. An ETNO has a large semi-major axis of at least 150–250 AU. The orbits of ETNOs are much less affected by the known giant planets than all other known trans-Neptunian objects. They may, however, be influenced by gravitational interactions with a hypothetical Planet Nine, shepherding these objects into similar types of orbits. The known ETNOs exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations.

    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.

    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.

    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.

    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 JM80". Minor Planet Center. Retrieved 9 October 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: (2014 JM80)" (2015-05-19 last obs.). Jet Propulsion Laboratory . Retrieved 9 October 2018.
    3. 1 2 3 Johnston, Wm. Robert (30 December 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 9 February 2018.
    4. ↑ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 9 February 2018.
    5. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    6. 1 2 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 9 February 2018.
    7. ↑ Jewitt, D; A, Morbidelli; H, Rauer; K, Altwegg; W, Benz; N, Thomas (2008). Trans-Neptunian objects and comets : Saas-Fee Advanced Course 35. Swiss society for astrophysics and astronomy . Berlin New York: Springer. p.  86. ISBN   978-3-540-71957-1. OCLC   261225528.
    8. ↑ 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.
    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. (Discovery paper)
    10. ↑ 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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