(445473) 2010 VZ98

From Wikipedia, the free encyclopedia
Jump to: navigation, search
(445473) 2010 VZ98
Discovery [1]
Discovered by D. L. Rabinowitz
M. E. Schwamb
S. Tourtellotte
Discovery site La Silla Obs.
Discovery date 11 November 2010
Designations
MPC designation (445473) 2010 VZ98
2010 VZ98
TNO[1] · SDO[2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 2
Observation arc 16.90 yr (6,171 days)
Aphelion 266.63 AU
Perihelion 34.333 AU
150.48 AU
Eccentricity 0.7719
1846.03 yr (674,262 days)
358.00°
0° 0m 1.8s / day
Inclination 4.5110°
117.39°
313.88°
Physical characteristics
Dimensions 401.33 km (calculated)[3]
461 km (assumed)[4]
9.72±0.05 h[3][5]
0.07 (assumed)[4]
0.10 (assumed)[3]
C[3]
4.81±0.04 (S)[5] · 5.1[1][3]

(445473) 2010 VZ98 is a trans-Neptunian object in the scattered disc, orbiting the Sun in the outermost parts of the Solar System.

It was discovered on 11 November 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observatory site in northern Chile,[6] when it was 38 AU from the Sun. With an absolute magnitude of approximately 5.0 and a calculated diameter above 400 kilometers, it is possibly a dwarf planet.[4]

Orbit and classification[edit]

The carbonaceous TNO orbits the Sun at a distance of 34.3–266.6 AU once every 1846 years (674,262 days). Its orbit has an eccentricity of 0.77 and an inclination of 5° with respect to the ecliptic.[1] Small number statistics suggest that this body may be trapped in a 3:2 orbital resonance with an unseen planet beyond Neptune with a semi-major axis of 195–215 AU.[7] The first precovery was taken by the Sloan Digital Sky Survey at the Apache Point Observatory in 1998, extending the body's observation arc by 12 years prior to its discovery. The precoveries were found in May 2015 (MPS 604632).[6]

Physical characteristics[edit]

A rotational lightcurve of 2010 VZ98 was obtained from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rotation period of 9.72±0.05 hours with a brightness variation of 0.18 magnitude (U=n.a.).[5]

While American astronomer Michael E. Brown assumes a diameter of 461 kilometers and an albedo of 0.07,[4] the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and calculates a diameter of 401 kilometers.[3]

Naming[edit]

As of 2017, this minor planet remains unnamed.[6]

See also[edit]

References[edit]

  1. ^ a b c d e "JPL Small-Body Database Browser: 445473 (2010 VZ98)" (2015-10-12 last obs.). Jet Propulsion Laboratory. Retrieved 2 June 2017. 
  2. ^ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2012-08-31. 
  3. ^ a b c d e f "LCDB Data for (445473)". Asteroid Lightcurve Database (LCDB). Retrieved 7 September 2016. 
  4. ^ a b c d Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 7 September 2016. 
  5. ^ a b c Benecchi, Susan D.; Sheppard, Scott S. (May 2013). "Light Curves of 32 Large Transneptunian Objects" (PDF). The Astronomical Journal. 145 (5): 19. arXiv:1301.5791Freely accessible. Bibcode:2013AJ....145..124B. doi:10.1088/0004-6256/145/5/124. Retrieved 7 September 2016. 
  6. ^ a b c "445473 (2010 VZ98)". Minor Planet Center. Retrieved 7 September 2016. 
  7. ^ de la Fuente Marcos, C.; de la Fuente Marcos, R. (September 2014). "Extreme trans-Neptunian objects and the Kozai mechanism: signalling the presence of trans-Plutonian planets". Monthly Notices of the Royal Astronomical Society: Letters. 443 (1): L59–L63. arXiv:1406.0715Freely accessible. Bibcode:2014MNRAS.443L..59D. doi:10.1093/mnrasl/slu084. Retrieved 7 September 2016. 

External links[edit]