(55638) 2002 VE95

(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]

(55638) 2003 VE95
Discovery[1]
Discovered byNEAT
Discovery date14 November 2002
Designations
2002 VE95
Plutino[2]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 2
Observation arc9246 days (25.31 yr)
Earliest precovery date12 October 1990
Aphelion50.167 AU (7.5049 Tm) (Q)
Perihelion27.943 AU (4.1802 Tm) (q)
39.055 AU (5.8425 Tm) (a)
Eccentricity0.28452 (e)
244.07 yr (89148.1 d)
26.267° (M)
0° 0m 14.538s / day (n)
Inclination16.337° (i)
199.87° (Ω)
206.37° (ω)
Earth MOID26.9598 AU (4.03313 Tm)
Jupiter MOID22.9846 AU (3.43845 Tm)
Physical characteristics
Dimensions249.8+13.5
−13.1[4]
6.76 h (0.282 d)
9.97 h (0.415 d) (ambiguous)[5]
6–9 h[6]
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[7]
5.70±0.06,[4] 5.3[3]

    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 291 times over 19 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.[6]

    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.[8]

    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.[9] The spectral behavior of this object is similar to 5145 Pholus, a centaur.[9] 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.[10]

    References
    1. "List Of Transneptunian Objects". IAU Minor Planet Center. Archived from the original on 27 October 2010. Retrieved 2011-01-08.
    2. "MPEC 2008-O05 : Distant Minor Planets". Minor Planet Center & Tamkin Foundation Computer Network. 2008-07-17. Retrieved 2008-07-23.
    3. "JPL Small-Body Database Browser: (55638) 2003 VE95" (2017-03-16 last obs). Retrieved 6 January 2019.
    4. 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. Thirouin, A.; Ortiz, J. L.; Duffard, R.; Santos-Sanz, P.; Aceituno, F. J.; Morales, N. (October 2010). "Short-term variability of a sample of 29 trans-Neptunian objects and Centaurs" (PDF). Astronomy and Astrophysics. 522: A93. Bibcode:2010A&A...522A..93T. doi:10.1051/0004-6361/200912340.
    6. 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. (eds.). The Solar System Beyond Neptune (pdf). University of Arizona Press. pp. 129–142. ISBN 978-0-8165-2755-7.
    7. "AstDys 2002VE95 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2010-08-05.
    8. 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.
    9. 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.
    10. 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.