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(341843) 2008 EV5

Summary

(341843) 2008 EV5, provisional designation 2008 EV5, is a sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid of the Aten group, approximately 400 metres (1,300 feet) in diameter. It was discovered on 4 March 2008, by astronomers of the Mount Lemmon Survey at Mount Lemmon Observatory near Tucson, Arizona, United States.[1]

(341843) 2008 EV5
Diagram of 2008 EV5's Earth-crossing orbit
Discovery[1]
Discovered byMount Lemmon Srvy.
Discovery siteMount Lemon Obs.
Discovery date4 March 2008
Designations
(341843) 2008 EV5
2008 EV5
NEO · Aten · PHA[1][2]
Orbital characteristics[2]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 1
Observation arc2.10 yr (768 days)
Aphelion1.0383 AU
Perihelion0.8783 AU
0.9583 AU
Eccentricity0.0835
0.94 yr (343 days)
213.55°
1° 3m 2.16s / day
Inclination7.4368°
93.390°
234.81°
Earth MOID0.0149 AU (5.8 LD)
Physical characteristics
Dimensions(420 × 410 × 390) m[3]
Mean diameter
0.370±0.006 km[4]
0.400±0.014 km[5]
0.400±0.034 km[6]
0.400±0.050 km[3][6]
3.717±0.008 h[7]
3.725 h[8]
3.7255±0.002 h[9]
7.2 h[10]
10.200±0.002 h[8]
0.104±0.312[6]
0.12±0.04[3]
0.13±0.05[4]
0.137±0.013[6]
0.1373±0.0129[5]
X[11] · C[12] · S (assumed)[8]
19.7[5][6] · 19.91[8] · 20.0[2] · 20.0±0.4[4]

Origin and orbital history edit

2008 EV5 started its existence as part of a much larger body in the asteroid belt, with a likely diameter greater than 100 kilometers.[13] 2008 EV5's immediate history likely started when its parent body experienced a large cratering event or, more likely, a catastrophic disruption event that resulted in a highly fractured, shattered, or reaccumulated object (rubble pile). As a result, 2008 EV5 may have been produced as a reassembly of ejected fragments. The location of what is now 2008 EV5 within this parent body is unknown.[14]

Given the available modeling work and data, the most plausible source family candidates for 2008 EV5 are Eulalia, New Polana, and Erigone. This assumes that 2008 EV5's true albedo is considerably lower than 10%. If it does have a high albedo, a plausible source would be a population of high-albedo C-type asteroids in the inner asteroid belt. Second tier candidate families for the high-albedo case are Baptistina and Pallas.[14]

From here, the newly liberated 2008 EV5 began to change via the forces referred to as the Yarkovsky and YORP effects. The Yarkovsky effect describes a small force that affects orbital motion. It is caused by sunlight; when objects heat up in the Sun, they reradiate the energy away as heat, which in turn creates a tiny thrust. This recoil acceleration is much weaker than solar and planetary gravitational forces, but it can produce substantial orbital changes over timescales ranging from many millions to billions of years. The same physical phenomenon also creates a thermal torque that probably caused 2008 EV5 to take on a top-like appearance.[3][14][15]

Dynamical models indicate that 2008 EV5 migrated inward across the inner asteroid belt over long timescales (i.e. the order of ~0.01–1 Gyr) until it reached a planetary gravitational resonance that drove it into the near-Earth asteroid (NEA) population over a timescale of the order of ~1 Myr. From there, gravitational interactions with both the planets and resonances allowed it to reach its current orbit within a few Myr to a few tens of Myr.[14]

Close approaches edit

On 23 December 2008, 2008 EV5 made a close approach to Earth at a distance of 8.4 lunar distances (0.022 AU, 3.2 million km), its closest until 2169.[3] Its brightness peaked on 26 December about 13.2 magnitude.

 
2008 Path of 2008 EV5 close approach, with 3 day motion markers
Earth Approach on 20 December 2023[2]
Date JPL Horizons
nominal geocentric
distance (AU) 		uncertainty
region
(3-sigma)
2023-Dec-20 06:52 0.04226 AU (6.322 million km)[2] ±1741 km[16]

Physical characteristics edit

 
Radar-based shape model of 2008 EV5

2008 EV5 is an oblate spheroid (also described as "muffin-shaped"[17]) 400 m (1,300 ft) in diameter. It rotates very slowly in a retrograde direction. There is a 150 m (490 ft) diameter concave feature, possibly an impact crater, or a relic feature from a previous episode of rapid rotation that caused the asteroid's shape to reconfigure.[3]

Visible and near-infrared spectroscopy show that 2008 EV5's composition is similar to that of carbonaceous chondrite meteorites.[12]

Proposed sample return mission edit

2008 EV5 was the preliminary baseline target of NASA's proposed sample-return Asteroid Redirect Mission. Besides 2008 EV5, several other asteroids, including Itokawa and Bennu, were considered for this mission,[18][19] before its cancellation in 2017.

See also edit

References edit

  1. ^ a b c "341843 (2008 EV5)". Minor Planet Center. Retrieved 17 January 2018.
  2. ^ a b c d e "JPL Small-Body Database Browser: 341843 (2008 EV5)" (2010-04-11 last obs.). Jet Propulsion Laboratory. Retrieved 17 January 2018.
  3. ^ a b c d e f Busch, Michael W.; Ostro, Steven J.; Benner, Lance A. M.; Brozovic, Marina; Giorgini, Jon D.; Jao, Joseph S.; et al. (April 2011). "Radar observations and the shape of near-Earth ASTEROID 2008 EV5" (PDF). Icarus. 212 (2): 649–660. arXiv:1101.3794. Bibcode:2011Icar..212..649B. doi:10.1016/j.icarus.2011.01.013. S2CID 56469588. Retrieved 17 January 2018.
  4. ^ a b c Alí-Lagoa, V.; Lionni, L.; Delbo, M.; Gundlach, B.; Blum, J.; Licandro, J. (January 2014). "Thermophysical properties of near-Earth asteroid (341843) 2008 EV5 from WISE data". Astronomy and Astrophysics. 561: 8. arXiv:1310.6715. Bibcode:2014A&A...561A..45A. doi:10.1051/0004-6361/201322215. S2CID 119268126.
  5. ^ a b c Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID 118700974.
  6. ^ a b c d e Mainzer, A.; Grav, T.; Bauer, J.; Masiero, J.; McMillan, R. S.; Cutri, R. M.; et al. (December 2011). "NEOWISE Observations of Near-Earth Objects: Preliminary Results". The Astrophysical Journal. 743 (2): 17. arXiv:1109.6400. Bibcode:2011ApJ...743..156M. doi:10.1088/0004-637X/743/2/156. S2CID 239991.
  7. ^ Skiff, Brian A.; Bowell, Edward; Koehn, Bruce W.; Sanborn, Jason J.; McLelland, Kyle P.; Warner, Brian D. (July 2012). "Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) - 2008 May through 2008 December". The Minor Planet Bulletin. 39 (3): 111–130. Bibcode:2012MPBu...39..111S. ISSN 1052-8091.
  8. ^ a b c d "LCDB Data for (341843)". Asteroid Lightcurve Database (LCDB). Retrieved 17 January 2018.
  9. ^ Galad, Adrian; Vilagi, Jozef; Kornos, Leonard; Gajdos, Stefan (July 2009). "Relative Photometry of Nine Asteroids from Modra". The Minor Planet Bulletin. 36 (3): 116–118. Bibcode:2009MPBu...36..116G. ISSN 1052-8091.
  10. ^ Behrend, Raoul. "Asteroids and comets rotation curves – (341843)". Geneva Observatory. Retrieved 17 January 2018.
  11. ^ Ye, Q.-z. (February 2011). "BVRI Photometry of 53 Unusual Asteroids". The Astronomical Journal. 141 (2): 32. arXiv:1011.0133. Bibcode:2011AJ....141...32Y. doi:10.1088/0004-6256/141/2/32. S2CID 119307210.
  12. ^ a b Reddy, Vishnu; Le Corre, Lucille; Hicks, Michael; Lawrence, Kenneth; Buratti, Bonnie J.; Abell, Paul A.; et al. (November 2012). "Composition of near-Earth Asteroid 2008 EV5: Potential target for robotic and human exploration". Icarus. 221 (2): 678–681. arXiv:1209.1207. Bibcode:2012Icar..221..678R. doi:10.1016/j.icarus.2012.08.035. S2CID 119243535.
  13. ^ Morbidelli, Alessandro; Bottke, William F.; Nesvorný, David; Levison, Harold F. (December 2009). "Asteroids were born big". Icarus. 204 (2): 558–573. arXiv:0907.2512. Bibcode:2009Icar..204..558M. doi:10.1016/j.icarus.2009.07.011. S2CID 12632943.
  14. ^ a b c d Mazanek, Daniel; Reeves, David. "Asteroid Redirect Mission (ARM) Formulation Assessment and Support Team (FAST) Final Report" (PDF). NASA Official. National Aeronautics and Space Administration. Retrieved 20 February 2016.   This article incorporates text from this source, which is in the public domain.
  15. ^ Walsh, Kevin J.; Richardson, Derek C.; Michel, Patrick (July 2008). "Rotational breakup as the origin of small binary asteroids". Nature. 454 (7201): 188–191. Bibcode:2008Natur.454..188W. doi:10.1038/nature07078. PMID 18615078. S2CID 4418744.
  16. ^ "Horizons Batch for 2023-12-20 Close Approach". JPL Horizons. Archived from the original on 26 October 2022. Retrieved 26 October 2022. RNG_3sigma = uncertainty range in km. (JPL#107/Soln.date: 2021-Apr-14 generates RNG_3sigma = 1741 km)
  17. ^ Wall, Mike (26 March 2015). "NASA wants to pluck a boulder from an asteroid. But which asteroid?". AP News. Retrieved 24 December 2018.
  18. ^ Steitz, David E. (25 March 2015). "RELEASE 15-050 - NASA Announces Next Steps on Journey to Mars: Progress on Asteroid Initiative". NASA. Retrieved 26 March 2015.
  19. ^ Borenstein, Seth (25 March 2015). "NASA details plans to pluck rock off asteroid, explore it". AP News. Retrieved 26 March 2015.

External links edit

  • Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
  • Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul
  • (341843) 2008 EV5 at NeoDyS-2, Near Earth Objects—Dynamic Site
    • Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
  • (341843) 2008 EV5 at ESA–space situational awareness
    • Ephemerides · Observations · Orbit · Physical properties · Summary
  • (341843) 2008 EV5 at the JPL Small-Body Database
    • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters

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