Discovery [1] | |
---|---|
Discovered by | Pan-STARRS 1 |
Discovery site | Haleakala Obs. |
Discovery date | 9 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]
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]
Discovery [1] | |
---|---|
Discovered by | Pan-STARRS 1 |
Discovery site | Haleakala Obs. |
Discovery date | 9 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]
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]