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2002 Ve68

2002 VE68
Discovery
Discovered by LONEOS
Discovery date November 11, 2002
Designations
MPC designation 2002 VE68
Aten asteroid,[1][2]
Mercury grazer,
Venus crosser,
Earth crosser
Orbital characteristics[2][3][4]
Epoch May 23, 2014 (JD 2456800.5)
(Uncertainty=0)
Aphelion 1.0205807900 ± 0.0000000007 AU (Q)
Perihelion 0.42675939 ± 0.00000003 AU (q)
0.7236700886 ± 0.0000000005 AU (a)
Eccentricity 0.41028461 ± 0.00000004
0.62 ± 0.0000000006 yr
83.51813±0.00002
Inclination 9.005790°±0.000011°
231.576924°±0.000005° (Ω)
355.458599°±0.000013° (ω)
Physical characteristics
Dimensions 210–470 m[1][5]
13.4 h[2]
20.5[2]

2002 VE68, also written 2002 VE68, is a temporary quasi-satellite of Venus.[6] It was the first quasi-satellite to be discovered around a major planet in the Solar System. In a frame of reference rotating with Venus, it appears to travel around it during one Venusian year but it actually orbits the Sun, not Venus.[7]

Contents

  • Discovery, orbit and physical properties 1
  • Quasi-satellite dynamical state and orbital evolution 2
  • Potentially hazardous asteroid 3
  • See also 4
  • Notes 5
  • References 6
  • External links 7

Discovery, orbit and physical properties

It was discovered on November 11, 2002 at Lowell Observatory. As of February 2013, 2002 VE68 has been observed telescopically 457 times with a data-arc span of 2,947 days and it was the target of Doppler observations in 5 occasions; therefore, its orbit is very well determined. Its semi-major axis (0.7237 AU) is very similar to that of Venus but its eccentricity is rather large (0.4104) and its orbital inclination is also significant (9.0060°). The spectrum of 2002 VE68 implies that it is an X-type asteroid and hence an albedo of about 0.25 should be assumed.[8] This combined with an absolute visual magnitude of 20.50 gives a diameter of about 200 m.[8] Its rotational period is 13.5 h and its light curve has an amplitude of 0.9 mag which hints at a very elongated body, perhaps a contact binary.[8]

Quasi-satellite dynamical state and orbital evolution

The existence of retrograde satellites or quasi-satellites was first considered by J. Jackson in 1913[9] but none was discovered until almost 100 years later.[7] 2002 VE68 was the first quasi-satellite to be discovered, in 2002, although it was not immediately recognized as such. 2002 VE68 was identified as a quasi-satellite of Venus by Seppo Mikkola, Ramon Brasser, Paul A. Wiegert and Kimmo Innanen in 2004, two years after the actual discovery of the object.[6][7] From the perspective of a hypothetical observer in a frame of reference rotating with Venus, it appears to travel around the planet during one Venusian year although it does not orbit Venus but the Sun like any other asteroid. As quasi-satellite, this minor body is trapped in a 1:1 mean-motion resonance with Venus. Besides being a Venus co-orbital, this Aten asteroid is also a Mercury grazer and an Earth crosser. 2002 VE68 exhibits resonant (or near-resonant) behavior with Mercury, Venus and Earth.[10][11] It seems to have been co-orbital with Venus for only the last 7,000 years, and is destined to be ejected from this orbital arrangement about 500 years from now.[7] During this time, its distance to Venus has been and will remain larger than about 0.2 AU (3·107 km).

Potentially hazardous asteroid

2002 VE68 is included in the Minor Planet Center list of Potentially Hazardous Asteroids (PHAs) because it comes relatively frequently to within 0.05 AU of Earth. Approaches as close as 0.04 AU occur with a periodicity of 8 years due to its near 8:13 resonance with Earth.[10] 2002 VE68 was discovered during the close approaches of November 11, 2002). During the last close encounter on November 7, 2010, 2002 VE68 approached Earth within 0.035 AU (13.6 Lunar distances), brightening below 15th magnitude. Its next fly-by with Earth will take place on November 4, 2018 at 0.038 AU (5,700,000 km; 3,500,000 mi).[12] Numerical simulations indicate that an actual collision with Earth during the next 10,000 years is not likely, although dangerously close approaches to about 0.002 AU are possible.[10]

See also

Notes

  1. ^ This is assuming an albedo of 0.25–0.05.

References

  1. ^ List Of Aten Minor Planets
  2. ^ a b c d 2002 VE68 at the JPL Small-Body Database
    • Discovery · Orbit diagram · Orbital elements · Physical parameters Retrieved 2011-09-13
  3. ^ AstDys-2 on 2002 VE68 Retrieved 2012-08-13
  4. ^ NEODyS-2 on 2002 VE68 Retrieved 2012-08-13
  5. ^ Absolute-magnitude conversion table (H)
  6. ^ a b Discovery of the first quasi-satellite of Venus (press announcement, Tuorla Observatory)
  7. ^ a b c d Asteroid 2002 VE68, a quasi-satellite of Venus
  8. ^ a b c Physical characterization of 2002 VE68, a quasi-moon of Venus
  9. ^ Retrograde satellite orbits
  10. ^ a b c On the dynamical evolution of 2002 VE68
  11. ^ de la Fuente Marcos, C.; de la Fuente Marcos, R. "Asteroid 2012 XE133, a transient companion to Venus".  
  12. ^ "JPL Close-Approach Data: (2002 VE68)" (2010-12-06 last obs (arc=8 years)). Retrieved 2013-01-05. 
Further reading
  • Retrograde satellite orbits, by Jackson, J. 1913, Monthly Notices of the Royal Astronomical Society, Vol. 74, pp. 62–82.
  • Understanding the Distribution of Near-Earth Asteroids Bottke, W. F., Jedicke, R., Morbidelli, A., Petit, J.-M., Gladman, B. 2000, Science, Vol. 288, Issue 5474, pp. 2190–2194.
  • A Numerical Survey of Transient Co-orbitals of the Terrestrial Planets Christou, A. A. 2000, Icarus, Vol. 144, Issue 1, pp. 1–20.
  • Debiased Orbital and Absolute Magnitude Distribution of the Near-Earth Objects Bottke, W. F., Morbidelli, A., Jedicke, R., Petit, J.-M., Levison, H. F., Michel, P., Metcalfe, T. S. 2002, Icarus, Vol. 156, Issue 2, pp. 399–433.
  • Asteroid 2002 VE68, a quasi-satellite of Venus, by Mikkola, S., Brasser, R., Wiegert, P., & Innanen, K. 2004, Monthly Notices of the Royal Astronomical Society, Vol. 351, Issue 3, pp. L63-L65.
  • Transient co-orbital asteroids Brasser, R., Innanen, K. A., Connors, M., Veillet, C., Wiegert, P., Mikkola, S., Chodas, P. W. 2004, Icarus, Vol. 171, Issue 1, pp. 102–109.
  • The population of Near Earth Asteroids in coorbital motion with Venus Morais, M. H. M., Morbidelli, A. 2006, Icarus, Vol. 185, Issue 1, pp. 29–38.
  • On the dynamical evolution of 2002 VE68, by de la Fuente Marcos, C., & de la Fuente Marcos, R. 2012, Monthly Notices of the Royal Astronomical Society, Vol. 427, Issue 1, pp. 728–739.
  • Asteroid 2012 XE133: a transient companion to Venus de la Fuente Marcos, C., de la Fuente Marcos, R. 2013, Monthly Notices of the Royal Astronomical Society, Vol. 432, Issue 2, pp. 886–893.

External links

  • 2002 VE68 data at MPC
  • List of Potentially Hazardous Asteroids (PHAs)
  • Image acquired during the last 2002 VE68 close approach, November 7, 2010 (Martin Mobberley's Astronomical Images web site)
  • Light curve (Ondřejov NEO Photometric Program)
  • 2002 VE68 Goldstone Radar Observations
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