(275809) 2001 QY297
| Discovery[1][2] | |
|---|---|
| Discovered by | Marc William Buie |
| Discovery date | 21 August 2001 |
| Designations | |
| MPC designation | (275809) 2001 QY297 |
| 2001 QY297 | |
| TNO (cubewano)[3] | |
| Orbital characteristics[2] | |
| Epoch 13 January 2013 (JD 2454100.5) | |
| Aphelion | 47.380 AU |
| Perihelion | 40.013 AU |
| 43.697 AU | |
| Eccentricity | 0.084 |
| 288.86 a | |
| 84.415° | |
| Inclination | 1.548° |
| 108.776° | |
| 123.591° | |
| Known satellites | 1 |
| Physical characteristics | |
| Dimensions |
229+22 −108 km (combined) 169+16 −80 km (primary) 154+15 −73 km (satellite)[4] |
| Mass | (4.105±0.038)×1018 kg[4] |
Mean density |
0.92+1.30 −0.27 g/cm3[4][lower-alpha 1] |
Sidereal rotation period | 11.68 [5] |
| Albedo |
0.152+0.439 −0.035[4] |
Spectral type |
V−R=0.43 ± 0.09 B−V=0.7[1] |
| 5.86 ± 0.31[6] | |
|
| |
(275809) 2001 QY297 is a binary classical Kuiper belt object belonging to the cold population.[4]
Discovery and orbit
(275809) 2001 QY297 was discovered on 21 August 2001 by Marc William Buie from Cerro Tololo Observatory, La Serena, Chile.[1][3] (275809) 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.[4]
Satellite
(275809) 2001 QY297 is a binary system consisting of two components of approximately equal size.[4] The satellite was discovered on 18 April 2006.[1] 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.[4]
| 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 (275809) 2001 QY297 appear to have a red color.[6] 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.[5]
Notes
- ↑ Assuming that both components have equal albedos and equal densities
References
- 1 2 3 4 Wm. Robert Johnston (23 June 2015). "(275809) 2001 QY297". Johnston's Archive. Retrieved 2016-03-09.
- 1 2 "JPL Small-Body Database Browser: 275809 (2001 QY297)" (2013-10-13 last obs). Retrieved 2016-03-09.
- 1 2 "MPEC G54: DISTANT MINOR PLANETS (2006 Apr. 25.0 TT) [27421-2007/05-R1]". IAU Minor Planet Center. 2006-04-14. Retrieved 2016-02-24.
- 1 2 3 4 5 6 7 8 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:2012A&A...541A..94V. doi:10.1051/0004-6361/201322416.
- 1 2 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. Bibcode:2014DPS....4642109T. doi:10.1051/0004-6361/201423567.
- 1 2 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.
- ↑ 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.
External links
- Orbital simulation from JPL (Java) / Ephemeris
- (275809) 2001 QY297 at the JPL Small-Body Database
| ||||||||||||||||||||||||||||
| ||||||||||||||