(55638) 2002 VE95

(55638) 2003 VE95
Discovery[1]
Discovered by NEAT
Discovery date 14 November 2002
Designations
MPC designation 2002 VE95
Plutino[2]
Orbital characteristics[3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 2
Observation arc 9246 days (25.31 yr)
Earliest precovery date 12 October 1990
Aphelion 50.686 AU (7.5825 Tm) (Q)
Perihelion 28.010 AU (4.1902 Tm) (q)
39.348 AU (5.8864 Tm) (a)
Eccentricity 0.28814 (e)
246.83 yr (90153.9 d)
20.605° (M)
0° 0m 14.376s / day (n)
Inclination 16.339° (i)
199.90° (Ω)
207.41° (ω)
Earth MOID 27.0273 AU (4.04323 Tm)
Jupiter MOID 23.0566 AU (3.44922 Tm)
Physical characteristics
Dimensions 249.8+13.5
−13.1[4]
6.76 h (0.282 d)
6–9 h[5]
0.149+0.019
−0.016[4]
B−V=1.07±0.14
V−R=0.72±0.05
B−R=1.79±0.04
R−I=0.76±0.12
V−I=1.38±0.15
B−I=2.47±0.13[4]
20.5[6]
5.70±0.06,[4] 5.6[3]

    (55638) 2002 VE95, also written as 2002 VE95, is a trans-Neptunian object (TNO) with an absolute magnitude of 5.7.[4] A 2:3 orbital resonance with Neptune makes it a plutino.[2]

    Orbit and rotation

    As a plutino 2002 VE95 is locked in 2:3 resonance with Neptune. This means that the ratio of their orbital periods is equal to 3/2.[2] It has been observed 190 times over 8 oppositions with precovery images back to 1990.[3]

    The rotation period of 2002 VE95 is unknown but it probably lies between 6 and 9 hours.[5]

    Physical characteristics

    The size of 2002 VE95 is estimated at 249.8+13.5
    −13.1     km    , based on the Herschel Space Telescope measurements of the thermal radiation coming from it.[4] In the visible light this object is from moderately red to very red in color (different observations produced different results) and has a featureless reflectance spectrum.[7]

    The near-infrared spectrum of 2002 VE95 is flat with two distinct absorption bands of water ice at 1.5 and 2.0 μm. There is the third feature near 2.3 μm of unclear origin.[8] The spectral behavior of this object is similar to 5145 Pholus, a centaur.[8] The surface of 2002 VE95 is heterogeneous—the amount of different ices and non-ice components depends on the observed area. Among the probable surface materials are water ice, methanol ice and various titan/triton tholins. The methanol ice is generally associated with redder areas. The surface of 2002 VE95 appears to be primordial in origin.[9]

    References

    1. ↑ "List Of Transneptunian Objects". IAU Minor Planet Center. Archived from the original on 27 October 2010. Retrieved 2011-01-08.
    2. 1 2 3 "MPEC 2008-O05 : Distant Minor Planets". Minor Planet Center & Tamkin Foundation Computer Network. 2008-07-17. Retrieved 2008-07-23.
    3. 1 2 3 "JPL Small-Body Database Browser: (55638) 2003 VE95" (2016-02-04 last obs). Retrieved 6 April 2016.
    4. 1 2 3 4 5 6 Mommert, Michael; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; Delsanti, A.; Vilenius, E.; Müller, T. G.; Peixinho, N.; Lellouch, E.; Szalai, N.; Henry, F.; Duffard, R.; Fornasier, S.; Hartogh, P.; Mueller, M.; Ortiz, J. L.; Protopapa, S.; Rengel, M.; Thirouin, A. (May 2012). "TNOs are cool: A survey of the trans-Neptunian region—V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy & Astrophysics. 541: A93. arXiv:1202.3657. Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562.
    5. 1 2 Sheppard, Scott S.; Lacerda, Pedro; Ortiz, Jose L. (2008). "Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities". In Barucci, M. Antonietta; Boehnhardt, H.; Cruikshank, D.P.; Morbidelli, A. The Solar System Beyond Neptune (pdf). University of Arizona Press. pp. 129–142. ISBN 978-0-8165-2755-7.
    6. ↑ "AstDys 2002VE95 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2010-08-05.
    7. ↑ Fornasier, S.; Barucci, M.A.; De Bergh, C.; Alvarez-Candal, A.; Demeo, F.; Merlin, F.; Perna, D.; Guilbert, A.; Delsanti, A.; Dotto, E.; Doressoundiram, A. (2009). "Visible spectroscopy of the new ESO large programme on trans-Neptunian objects and Centaurs: final results". Astronomy and Astrophysics. 508 (1): 457–465. arXiv:0910.0450. Bibcode:2009A&A...508..457F. doi:10.1051/0004-6361/200912582.
    8. 1 2 Barucci, M. A.; Merlin, F.; Dotto, E.; Doressoundiram, A.; De Bergh, C. (2006). "TNO surface ices Observations of the TNO 55638 (2002 VE95) and analysis of the population's spectral properties". Astronomy and Astrophysics. 455 (2): 725–730. Bibcode:2006A&A...455..725B. doi:10.1051/0004-6361:20064951.
    9. ↑ Barucci, M. A.; Merlin, F.; Perna, D.; Alvarez-Candal, A.; Müller, T.; Mommert, M.; Kiss, C.; Fornasier, S.; Santos-Sanz, P.; Dotto, E. (2012). "The extra red plutino (55638) 2002 VE95". Astronomy & Astrophysics. 539: A152. Bibcode:2012A&A...539A.152B. doi:10.1051/0004-6361/201118505.
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.