(82075) 2000 YW134

Last updated

(82075) 2000 YW134
(82075) 2000 YW134 hst.png
2000 YW134 imaged by the Hubble Space Telescope on 25 October 2002
Discovery [1] [2]
Discovered by Spacewatch
Discovery site Kitt Peak National Obs.
Discovery date26 December 2000
Designations
(82075) 2000 YW134
2000 YW134 ·2001 XG201 [3]
TNO [4]  · res (3:8) [5] [6]
Orbital characteristics [4]
Epoch 1 July 2021 (JD 2459396.5)
Uncertainty parameter 2 [2] [4]
Observation arc 20.19 yr (7,373 d)
Aphelion 73.783 AU
Perihelion 40.999 AU
57.391 AU
Eccentricity 0.2856
434.78 yr (158,805 d)
35.927°
0° 0m 8.28s / day
Inclination 19.866°
127.00°
314.98°
Known satellites S/2005 (82075) 1
(Ds/Dp: 0.347) [7]
Physical characteristics
Mean diameter
>0.08 [8]
0.408±0.329 [5] [7]
21.54 [11]
4.72 [2] [4]

    (82075) 2000 YW134 (provisional designation 2000 YW134) is a resonant trans-Neptunian object and binary system, located in the outermost region of the Solar System. It was discovered on 26 December 2000, by astronomers with the Spacewatch survey at Kitt Peak Observatory near Tucson, Arizona. The reddish object stays in a rare 3:8 resonance with Neptune. A smaller companion was discovered by the Hubble Space Telescope in October 2002. [7] As of 2021, neither the primary body nor its satellite have been named. [2]

    Contents

    Orbit and classification

    2000 YW134 orbits the Sun at a distance of 41.0–73.8  AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic. [4] The body's observation arc begins with its official discovery observation by Spacewatch on 26 December 2000. [2] It last came to perihelion in 1979, [12] and is currently at about 46.5 AU from the Sun, with an apparent magnitude of 21.54. [11] It will reach aphelion in December 2197. [12]

    2000 YW134 is a resonant trans-Neptunian object that stays in a rare 3:8 mean-motion orbital resonance with Neptune, orbiting exactly three times the Sun for every 8 orbits Neptune does. [6] There are currently two other objects known to have the same resonant type: 2014 UE228 and (542258) 2013 AP183 . [5] [13] Due to its relatively large distance to Neptune, a classification as an extended-scattered or detached object was also considered earlier on (Lykawka, 2006). However, improved observations and long-term numerical integrations of the object's orbit by Emel’yanenko and Kiseleva (84% probability) and the Deep Ecliptic Survey – with all alternative integrations in agreement, showing a minimum perihelion distance of 38.2 AU – have since secured its 3:8 orbital resonance with Neptune. [6] [14]

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 4 May 2004, receiving the number (82075) in the minor planet catalog ( M.P.C. 51853). [15] As of 2021, it has not been named. [2] According to the established naming conventions, it will be given a mythological name associated with the underworld. [16]

    Physical characteristics

    The surface of 2000 YW134 is moderately red in the visible part of the spectrum. Its IR spectral type transitions from the very red (RR) to the intermediate blue-red (BR). [10] Alternatively a BR-spectral type has also been assumed. [7] The object's B−V and V–R color indices have also been measured several times, giving an averaged value of close to 1.0 and 0.5, respectively, for a combined B−R magnitude of 1.50. [9]

    Diameter and albedo

    In 2010, observations with the Herschel Space Observatory constrained the object's geometric albedo to no darker than 8%, and allowed to place an upper limit to its effective mean-diameter of 500 km (310 mi), as no thermal radiation had been detected. [8] However, according to Michael Mommert's dissertation in 2013, the object has a much higher albedo of 0.408±0.329, which greatly reduces its effective diameter to 229 km (140 mi). [7]

    Satellite

    On 25 October 2002, observations in the far-infrared with the NICMOS instrument of the Hubble Space Telescope revealed that 2000 YW134 is a binary system with a satellite in its orbit. The discovery was announced on 6 October 2005. [7] [17] : 22  Johnston's Archive derives a diameter of 216 km (130 mi) for the primary and a diameter of 75 km (47 mi) for the secondary, based on a secondary-to-primary diameter ratio of 0.347, for a difference of 1.3 magnitudes between the two objects. The satellite, designated S/2005 (82075) 1, orbits its primary every 10 days (estimated) at an average distance of 1,900 km (1,200 mi). [7]

    Related Research Articles

    <span class="nowrap">1998 WW<sub>31</sub></span>

    1998 WW31, is a non-resonant trans-Neptunian object and binary system from the Kuiper belt located in the outermost region of the Solar System, approximately 148 kilometers (92 miles) in diameter. It was first observed on 18 November 1998, by American astronomer Marc Buie and Robert Millis at the Kitt Peak National Observatory in Arizona, United States. In December 2000, a minor-planet moon, designated S/2000 (1998 WW31) 1 with a diameter of 123 kilometers (76 miles), was discovered in its orbit. After Charon in 1978, it was the first of nearly 100 satellites since discovered in the outer Solar System.

    <span class="nowrap">(48639) 1995 TL<sub>8</sub></span>

    (48639) 1995 TL8 is a binary trans-Neptunian object from the scattered disc in the outermost regions of the Solar System. It was discovered by Arianna Gleason in 1995 and measures approximately 176 kilometers in diameter. Its 80-kilometer minor-planet moon, provisionally designated S/2002 (48639) 1, was discovered on 9 November 2002.

    (119070) 2001 KP77 (provisional designation 2001 KP77) is a resonant trans-Neptunian object in the Kuiper belt, a circumstellar disc located in the outermost region of the Solar System. It was discovered on 23 May 2001, by American astronomer Marc Buie at the Cerro Tololo Observatory in Chile. The object is locked in a 4:7 orbital resonance with Neptune. It has a red surface color and measures approximately 176 kilometers (110 miles) in diameter. As of 2021, it has not been named.

    <span class="mw-page-title-main">174567 Varda</span> Trans-Neptunian object

    174567 Varda (provisional designation 2003 MW12) is a binary trans-Neptunian planetoid of the resonant hot classical population of the Kuiper belt, located in the outermost region of the Solar System. Its moon, Ilmarë, was discovered in 2009.

    <span class="nowrap">(15875) 1996 TP<sub>66</sub></span>

    (15875) 1996 TP66 (provisional designation 1996 TP66) is a resonant trans-Neptunian object of the plutino population, located in the outermost region of the Solar System, approximately 154 kilometers (96 miles) in diameter. It was discovered on 11 October 1996, by astronomers Jane Luu, David C. Jewitt and Chad Trujillo at the Mauna Kea Observatories, Hawaii, in the United States. The very reddish RR-type with a highly eccentric orbit has been near its perihelion around the time of its discovery. This minor planet was numbered in 2000 and has since not been named. It is probably not a dwarf planet candidate.

    (95625) 2002 GX32 (provisional designation 2002 GX32) is a trans-Neptunian object that resides in the Kuiper belt. It has a 3:7 resonance with Neptune. It was discovered on April 8, 2002 by Marc W. Buie, Amy B. Jordan, and James L. Elliot.

    (118228) 1996 TQ66 (provisional designation 1996 TQ66) is a resonant trans-Neptunian object of the plutino population in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 October 1996, by American astronomers Jun Chen, David Jewitt, Chad Trujillo and Jane Luu, using the UH88 telescope at the Mauna Kea Observatories, Hawaii. The very red object measures approximately 185 kilometers (110 miles) in diameter. As of 2021, it has not been named.

    (118378) 1999 HT11 (provisional designation 1999 HT11) is a trans-Neptunian object from the outermost region of the Solar System, locked in a 4:7 orbital resonance with Neptune. It was discovered on 17 April 1999, by astronomers at the Kitt Peak Observatory, Arizona, in the United States. The very red object measures approximately 134 kilometers (83 miles) in diameter. As of 2021, it has not been named.

    (91205) 1998 US43 (provisional designation 1998 US43) is a resonant trans-Neptunian object of the plutino group, located in the Kuiper belt in the outermost region of the Solar System. The rather bluish body measures approximately 111 kilometers (69 miles) in diameter. It was discovered on 22 October 1998, by American astronomer Marc Buie at the Kitt Peak National Observatory in the United States. It is probably not a dwarf planet candidate.

    (35671) 1998 SN165 (provisional designation 1998 SN165) is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.

    <span class="nowrap">(145480) 2005 TB<sub>190</sub></span>

    (145480) 2005 TB190 (provisional designation 2005 TB190) is a trans-Neptunian object (TNO) with an absolute magnitude of 4.4.

    (131696) 2001 XT254, provisionally known as 2001 XT254, is a Kuiper belt object (KBO) that has a 3:7 resonance with Neptune.

    <span class="nowrap">(528381) 2008 ST<sub>291</sub></span>

    (528381) 2008 ST291, provisional designation 2008 ST291, is a 1:6 resonant trans-Neptunian object located in the outermost region of the Solar System that takes almost a thousand years to complete an orbit around the Sun. It was discovered on 24 September 2008 by American astronomers Megan Schwamb, Michael Brown and David Rabinowitz at the Palomar Observatory in California, with no known earlier precovery images.

    (55638) 2002 VE95 (provisional designation 2002 VE95) is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino population, locked in a 2:3 resonance with Neptune. The object is likely of primordial origin with a heterogeneous surface and a notably reddish color (RR) attributed to the presence of methanol and tholins. It has a poorly defined rotation period of 6.8 hours and measures approximately 250 kilometers (160 miles) in diameter, too small to be a dwarf planet candidate. As of 2021, it has not yet been named.

    (307463) 2002 VU130, prov. designation: 2002 VU130, is a trans-Neptunian object, located in the circumstellar disc of the Kuiper belt in the outermost region of the Solar System. The resonant trans-Neptunian object belongs to the population of plutinos and measures approximately 253 kilometers (160 miles) in diameter. It was discovered on 7 November 2002, by American astronomer Marc Buie at the Kitt Peak Observatory near Tucson, Arizona. The object has not been named yet.

    <span class="nowrap">(432949) 2012 HH<sub>2</sub></span>

    (432949) 2012 HH2 is a resonant trans-Neptunian object, approximately 255 kilometers (160 miles) in diameter, located in the outermost region of the Solar System. It was discovered by Slovak astronomer Tomáš Vorobjov from images taken on the night of 19 April 2012, at the Astronomical Research Institute (H21) in Illinois, United States. This minor planet was numbered (432949) by the Minor Planet Center on 4 April 2015 (M.P.C. 93615). As of 2021, it has not been named.

    <span class="nowrap">(523794) 2015 RR<sub>245</sub></span>

    (523794) 2015 RR245, provisional designation 2015 RR245, is a large trans-Neptunian object of the Kuiper belt in the outermost regions of the Solar System. It was discovered on 9 September 2015, by the Outer Solar System Origins Survey at Mauna Kea Observatories on the Big island of Hawaii, in the United States. The object is in a rare 2:9 resonance with Neptune and measures approximately 600 kilometers in diameter. 2015 RR245 was suspected to have a satellite according to a study announced by Noyelles et al. in a European Planetary Science Congress meeting in 2019.

    (523764) 2014 WC510 (provisional designation 2014 WC510) is a binary trans-Neptunian object discovered on 8 September 2011 by the Pan-STARRS survey at the Haleakalā Observatory in Hawaii. It was found by Pan-STARRS on 20 November 2014 and was announced later in July 2016 after additional observations and precovery identifications. It is in the Kuiper belt, a region of icy objects orbiting beyond Neptune in the outer Solar System. It is classified as a plutino, a dynamical class of objects in a 2:3 orbital resonance with Neptune. On 1 December 2018, a team of astronomers observed a stellar occultation by the object, which revealed that it is a compact binary system consisting of two separate components in close orbit around each other. The primary and secondary components are estimated to have diameters of around 180 km (110 mi) and 140 km (87 mi), respectively.

    2014 UE228 is a trans-Neptunian object from the outermost region of the Solar System. The object is in a rare 3:8 resonance with Neptune and measures approximately 93 kilometers (58 miles) in diameter. It was first observed on 22 October 2014, by astronomers with the Outer Solar System Origins Survey at the Mauna Kea Observatories, Hawaii, and was provisionally designated 2014 UE228. As of 2021, it has not been numbered.

    References

    1. ↑ "MPEC 2001-B03 : 2000 YW134". Minor Planet Electronic Circular . Minor Planet Center. 16 January 2001. Retrieved 9 September 2021.
    2. 1 2 3 4 5 6 "82075 (2000 YW134)". Minor Planet Center. Retrieved 9 September 2021.
    3. ↑ "MPEC 2002-A26 : 2000 YW134 = 2001 XG201". Minor Planet Electronic Circular. Minor Planet Center. 7 January 2002. Retrieved 9 September 2021.
    4. 1 2 3 4 5 "JPL Small-Body Database Browser: 82075 (2000 YW134)" (2021-03-04 last obs.). Jet Propulsion Laboratory . Retrieved 9 September 2021.
    5. 1 2 3 4 "List of Known Trans-Neptunian Objects". Johnston's Archive. 18 August 2020. Retrieved 9 September 2021.
    6. 1 2 3 "Orbit Fit and Astrometric record for 82075". Southwest Research Institute . Retrieved 9 September 2021.
    7. 1 2 3 4 5 6 7 8 9 10 Johnston, Wm. Robert (20 September 2014). "Asteroids with Satellites Database – (82075) 2000 YW134". Johnston's Archive. Retrieved 9 September 2021. Mommert, M., 2013, p.164 and Grundy, 2012
    8. 1 2 Müller, T. G.; Lellouch, E.; Stansberry, J.; Kiss, C.; Santos-Sanz, P.; Vilenius, E.; et al. (July 2010). "TNOs are Cool: A survey of the trans-Neptunian region. I. Results from the Herschel science demonstration phase (SDP)". Astronomy and Astrophysics. 518: L146. arXiv: 1005.2923 . Bibcode:2010A&A...518L.146M. doi:10.1051/0004-6361/201014683. ISSN   0004-6361. S2CID   118635387.
    9. 1 2 3 4 "LCDB Data for (82075)". Asteroid Lightcurve Database (LCDB). Retrieved 9 September 2021.
    10. 1 2 Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Dovgopol, Anatolij N. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus. 250: 482–491. Bibcode:2015Icar..250..482B. doi:10.1016/j.icarus.2014.12.004. ISSN   0019-1035.
    11. 1 2 "Asteroid (82075) 2000 YW134 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site. Retrieved 9 September 2021.
    12. 1 2 "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. Retrieved 8 September 2021.
    13. ↑ "The Deep Ecliptic Survey Object Classifications". Southwest Research Institute . Retrieved 9 September 2021.
    14. ↑ Emel'Yanenko, V. V.; Kiseleva, E. L. (April 2008). "Resonant motion of trans-Neptunian objects in high-eccentricity orbits". Astronomy Letters. 34 (4): 271–279. Bibcode:2008AstL...34..271E. doi:10.1134/S1063773708040075. ISSN   0320-0108. S2CID   122634598.
    15. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 9 September 2021.
    16. ↑ "Naming of Astronomical Objects – Minor planets". IAU – International Astronomical Union. Retrieved 27 July 2021.
    17. ↑ Stephens, Denise C.; Noll, Keith S. (February 2006). "Detection of Six Trans-Neptunian Binaries with NICMOS: A High Fraction of Binaries in the Cold Classical Disk". The Astronomical Journal. 131 (2): 1142–1148. arXiv: astro-ph/0510130 . Bibcode:2006AJ....131.1142S. doi:10.1086/498715. ISSN   0004-6256. S2CID   18812367.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.