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(121514) 1999 UJ7

From Wikipedia, the free encyclopedia

(121514) 1999 UJ7
Discovery[1]
Discovered by30 October 1999 by LINEAR
Discovery siteSocorro
Discovery date30 October 1999
Designations
2002 AC180[1]
Martian L4
Martian L4
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc21861 days (59.85 yr)
Aphelion1.5843517 AU (237.01564 Gm)
Perihelion1.4644704 AU (219.08165 Gm)
1.5244110 AU (228.04864 Gm)
Eccentricity0.0393206
1.88 yr (687.47 d)
229.9277°
0° 31m 25.183s / day
Inclination16.75044°
347.37714°
48.35771°
Earth MOID0.47372 AU (70.868 Gm)
Jupiter MOID3.49473 AU (522.804 Gm)
Physical characteristics
Dimensions~1 km[2]
X[3]
16.9[1]

(121514) 1999 UJ7 is a small asteroid orbiting near the L4 point of Mars (60 degrees ahead Mars on its orbit).[2] As of April 2024, it is one of only two known asteroids to orbit the leading L4 point of Mars — the other being 2023 FW14[4] — although at least 15 other asteroids orbit Mars's trailing L5 point: The largest being 5261 Eureka, (101429) 1998 VF31, and 2007 NS2.[2] Not only does (121514) 1999 UJ7 orbit on the other side of Mars from other similar asteroids, its spectrum is different as well, which is puzzling because all of the Martian trojans seem to be in very stable orbits.[3]

Orbit

Animation of 1999 UJ7 relative to Sun and Mars 1600-2500
   Sun ·   1999 UJ7 ·   Mars

(121514) 1999 UJ7 orbits around the L4 point of Mars in a very stable orbit and is large enough that the Yarkovsky effect will not affect its orbit.[2]

Physical characteristics

Due to similarity in the measured brightness of (121514) 1999 UJ7 with other Martian trojans, it is thought to be a small asteroid with an effective diameter on the order of 1 kilometer (0.62 mi).[2] Its spectrum suggests that it is an X-type asteroid, which is different from 5261 Eureka and 1998 VF31,[3] and is somewhat puzzling since different mineral compositions suggest different origins for the two groups of asteroids. The long lifetime of the orbits for these asteroids makes the possibility of one or more of them being interlopers unlikely, however. This suggests that either one or more of the Martian trojans was captured in such a way as to give it a long-term stable orbit (and it is therefore not a primordial Martian asteroid), or that some fusion or combination of previous asteroids resulted in the presently observed ones.[3] The Yarkovsky effect may provide a potential capture mechanism but not enough is known about the shapes of these objects to provide a useful Yarkovsky model.[3]

See also

References

  1. ^ a b c d "JPL Small-Body Database Browser: 121514 (1999 UJ7)". NASA/Jet Propulsion Laboratory. Retrieved 7 April 2016.
  2. ^ a b c d e Scholl, H.; Marzari, F.; Tricarico, P. (June 2005). "Dynamics of Mars Trojans" (PDF). Icarus. 175 (2): 397–408. Bibcode:2005Icar..175..397S. doi:10.1016/j.icarus.2005.01.018. Archived from the original (PDF) on 16 February 2012. Retrieved 22 April 2009.
  3. ^ a b c d e Rivkin, A. S.; Binzel, R. P.; Howell, E. S.; Bus, S. J.; Grier, J. A. (October 2003). "Spectroscopy and photometry of Mars Trojans". Icarus. 165 (2): 349–354. Bibcode:2003Icar..165..349R. doi:10.1016/S0019-1035(03)00211-2.
  4. ^ de la Fuente Marcos, Raúl; de León, Julia; de la Fuente Marcos, Carlos; Alarcon, Miguel R.; Licandro, Javier; Serra-Ricart, Miquel; Geier, Stefan; Cabrera-Lavers, Antonio (21 March 2024). "Dynamics of 2023 FW14, the second L4 Mars trojan, and a physical characterization using the 10.4 m Gran Telescopio Canarias". Astronomy & Astrophysics, Letters to the Editor. 683 (1): L14 (6 pages). arXiv:2403.04061. Bibcode:2024A&A...683L..14D. doi:10.1051/0004-6361/202449688.{{cite journal}}: CS1 maint: date and year (link)

External links

This page was last edited on 3 April 2024, at 20:28
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