(275809) 2001 QY297

(275809) 2001 QY297 is a trans-Neptunian object from the classical Kuiper belt, located in the outermost region of the Solar System. The binary classical Kuiper belt object belongs to the cold population.[5]

(275809) 2001 QY297
Hubble Space Telescope image of 2001 QY297 and its satellite, taken in 2006
Discovery[1]
Discovered byMarc Buie
Discovery date21 August 2001
Designations
Designation
(275809) 2001 QY297
2001 QY297
TNO [1] · cubewano[2][3]
cold
Orbital characteristics [1]
Epoch 13 January 2013 (JD 2454100.5)
Aphelion47.380 AU
Perihelion40.013 AU
43.697 AU
Eccentricity0.084
288.86 a
84.415°
Inclination1.548°
108.776°
123.591°
Known satellites1 (D: 154+15
−73 km[4][5]
Physical characteristics
Mean diameter
229+22
−108 km (effective)
169+16
−80 km (primary)
Mass(4.105±0.038)×1018 kg[5]
Mean density
0.92+1.30
−0.27 g/cm3[5][lower-alpha 1]
11.68 h[6]
Albedo0.152+0.439
−0.035[5]
Spectral type
V−R = 0.43±0.09
B−V = 0.7[4]
5.86±0.31[7]

    Discovery and orbit

    2001 QY297 was discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile.[4][2] 2001 QY297 belongs to the dynamically cold population of the classical Kuiper belt objects, which have small orbital eccentricities and inclinations. Their semi-major axes reside mainly in the interval 40–45 AU.[5]

    Satellite

    2001 QY297 is a binary system consisting of two components of approximately equal size.[5] The satellite was discovered on 18 April 2006.[4] Assuming that both components have the same albedo, the primary is estimated to be about 169 km in diameter. The size of the secondary (satellite) in this case is estimated at around 154 km. The total mass of the system is approximately 4×1018 kg. The average density of both components is about 1 g/cm3.[5]

    Orbital parameters of the (275809) 2001 QY297 system[8]
    Semi-major axis (km) Eccentricity Period (d) Inclination (°)
    9960 ± 31 0.4175 ± 0.0023 138.110 ± 0.023 172.86 ± 0.20

    Physical properties

    The surfaces of both components of 2001 QY297 appear to have a red color.[7] The object shows significant photometric variability with lightcurve amplitude of 0.49±0.03. The rotational period is either 5.84 or 11.68 hours.[6]

    Notes
    1. Assuming that both components have equal albedos and equal densities

    References
    1. "JPL Small-Body Database Browser: 275809 (2001 QY297)" (2013-10-13 last obs). Retrieved 9 March 2016.
    2. "MPEC G54: DISTANT MINOR PLANETS (2006 Apr. 25.0 TT) [27421-2007/05-R1]". IAU Minor Planet Center. 14 April 2006. Archived from the original on 4 March 2016. Retrieved 24 February 2016.
    3. Marc W. Buie. "Orbit Fit and Astrometric record for 275809". SwRI (Space Science Department). Retrieved 18 February 2018.
    4. Wm. Robert Johnston (23 June 2015). "(275809) 2001 QY297". Johnston's Archive. Retrieved 9 March 2016.
    5. Vilenius, E.; Kiss, C.; Mommert, M.; et al. (2014). ""TNOs are Cool": A survey of the trans-Neptunian region X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations". Astronomy & Astrophysics. 564: A35. arXiv:1403.6309. Bibcode:2014A&A...564A..35V. doi:10.1051/0004-6361/201322416.
    6. A. Thirouin; K.S. Noll; J.L. Ortiz; N. Morales (2014). "Rotational properties of the binary and non-binary populations in the trans-Neptunian belt". Astronomy & Astrophysics. 569: A3. arXiv:1407.1214. Bibcode:2014DPS....4642109T. doi:10.1051/0004-6361/201423567.
    7. Vilenius, E.; Kiss, C.; Mommert, M.; et al. (2014). ""TNOs are Cool": A survey of the trans-Neptunian region VI. Herschel>/PACS observations and thermal modeling of 19 classical Kuiper belt objects". Astronomy & Astrophysics. 541: A94. arXiv:1204.0697. Bibcode:2012A&A...541A..94V. doi:10.1051/0004-6361/201118743.
    8. Grundy, W. M.; Noll, K. S.; Nimmo, F.; Roe, H. G.; Buie, M. W.; Porter, S. B.; Benecchi, S. D.; Stephens, D. C.; Levison, H. F.; Stansberry, J. A. (2011). "Five new and three improved mutual orbits of transneptunian binaries" (pdf). Icarus. 213 (2): 678. arXiv:1103.2751. Bibcode:2011Icar..213..678G. doi:10.1016/j.icarus.2011.03.012.

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