(15875) 1996 TP66

Last updated

(15875) 1996 TP66
1996TP66-orbit.png
Orbital diagram with 1996 TP66 being well inside the orbit of Neptune as of 2008
Discovery [1]
Discovered by J. X. Luu
D. C. Jewitt
C. Trujillo
Discovery site Mauna Kea Obs.
Discovery date11 October 1996
Designations
(15875) 1996 TP66
1996 TP66
TNO [2]  · plutino [3] [4]
distant [1]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 3
Observation arc 12.03 yr (4,394 d)
Aphelion 51.960 AU
Perihelion 26.317 AU
39.139 AU
Eccentricity 0.3276
244.86 yr (89,435 d)
28.208°
0° 0m 14.4s / day
Inclination 5.7000°
316.68°
74.784°
Physical characteristics
Mean diameter
154±34  km [4] [5]
0.074 [4] [5]
RR [6]
B–V = 1.050 [6]
V–R = 0.660 [6]
V–I = 1.310 [6]
21.6 [7]
6.79±0.33 [8]
7.0 [1] [2]
7.39 [9] [10]
7.51±0.09 [5]

    (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. [1] 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.

    Contents

    Orbit and classification

    Plutino 1966TP66 20000y.jpg
    Plutino Resonance: motion of 1996 TP66 (red) and Pluto (grey) in a rotating frame with Neptune held stationary (equal to its orbital period)
    1996TP66 Distance to sun.jpg
    Distance to the Sun for 1996 TP66 (orange) Pluto (blue), and Neptune (pink) over a 1,000 year period

    1996 TP66 belongs to the dynamical population of plutinos, named after its largest member, Pluto. Plutinos are resonant trans-Neptunian objects in a 2:3 orbital resonance with Neptune, which means that they orbit the Sun exactly twice while Neptune orbits the Sun three times.

    It orbits the Sun at a distance of 26.3–52.0  AU once every 244 years and 10 months (89,435 days; semi-major axis of 39.14 AU). Its orbit has a notably high eccentricity of 0.33 and an inclination of 6° with respect to the ecliptic. [2] Among the plutinos, 1996 TP66 has one of the most elliptical orbits, with a perihelion almost halfway between Uranus (19.2 AU) and Neptune (30.1 AU). The body's observation arc begins with its official discovery observation at Mauna Kea in October 1996. [1] Calculations by the Minor Planet Center in 1997 showed that the eccentric orbit of 1996 TP66 comes within 6.9 AU of Uranus and stays more than 22.6 AU from Neptune over a 14,000-year period centered on the present. [11]

    Inside Neptune's orbit

    In 2000, this object came closest to the Sun (perihelion) at 26.3 AU, [2] and has since moved away to a distance of 29.2 AU by the end of 2018. [7] This means that this small plutino is still well inside the orbit of Neptune which has a semi-major axis of 30.1 AU.

    Like Pluto, this plutino spends part of its orbit closer to the Sun than Neptune. Like all resonant trans-Neptunian objects its orbit is dominated by Neptune. Simulations by the Deep Ecliptic Survey (DES) show that over the next 10 million years 1996 TP66 can acquire a perihelion distance (qmin) as small as 25.9 AU. [3] Objects like Huya and the plutino 2004 EW95 are also currently inside the orbit of Neptune.

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 26 July 2000 and received the number 15875 in the minor planet catalog ( M.P.C. 40993). [12] As of 2018, it has not been named. [1]

    Physical properties

    1996 TP66 has a RR taxonomic class, [4] [6] with "very red" surface in the visible (rather than a "neutral" or "grey-blue" one for objects of the BB class) and a flat featureless infrared spectrum. [8] [13] In 2015, Irina Belskaya published the following color indices: B–V (1.050), V–R (0.660) and V–I (1.310). [6] The resulting B–R magnitude is 1.71. [4] These indices agree with the results obtained by the Herschel Space Observatory (Mommert): B–V (1.030), V–R (0.660) and V–I (1.320), [5] and also agree with previous measurements by Olivier Hainaut: B–V (1.031), V–R (0.655) and V–I (1.324), [14] as well as B–V (0.984), V–R (0.654) and V–I (11.337) from in 2012 and 2002, respectively. [15] The numerous results are summarized at the Small Body Data Ferret. [16]

    Diameter and albedo

    According to the survey carried out by the Herschel Space Telescope using its PACS instrument, 1996 TP66 measures 154.0+28.8
    −33.7     kilometers in diameter and its surface has an albedo of 0.074+0.063
    −0.031    . [5] The results supersedes a previous study that gave a much larger diameter of 350 kilometers with a lower albedo of 0.03. [17] According to Michael Brown, it is "probably not" a dwarf planet candidate, due to its relatively small diameter estimated at 158 kilometers. [18] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and derives a diameter of 139.81 kilometers based on an absolute magnitude of 7.39. [9]

    Rotation period

    1996 TP66 was part of a rotational lightcurve study which was published in the journal Nature in 1999. The photometric observations gave a brightness variation of no more than 0.12 magnitude, which is indicative of a rather spherical shape. [10] [16] As of 2018, the body's rotation period and pole remain unknown. [9]

    Related Research Articles

    <span class="mw-page-title-main">38628 Huya</span> Trans-Neptunian object

    38628 Huya ( hoo-YAH; provisional designation 2000 EB173) is a binary trans-Neptunian object located in the Kuiper belt, a region of icy objects orbiting beyond Neptune in the outer Solar System. Huya is classified as a plutino, a dynamical class of trans-Neptunian objects with orbits in a 3:2 orbital resonance with Neptune. It was discovered by the Quasar Equatorial Survey Team and was identified by Venezuelan astronomer Ignacio Ferrín in March 2000. It is named after Juyá, the mythological rain god of the Wayuu people native to South America.

    <span class="nowrap">(55565) 2002 AW<sub>197</sub></span> Classical Kuiper belt object

    (55565) 2002 AW197 (provisional designation 2002 AW197) is a classical, non-resonant trans-Neptunian object from the Kuiper belt in the outermost region of the Solar System, also known as a cubewano. With a likely diameter of at least 700 kilometers (430 miles), it is approximately tied with 2002 MS4 and 2013 FY27 (to within measurement uncertainties) as the largest unnamed object in the Solar System. It was discovered at Palomar Observatory in 2002.

    <span class="mw-page-title-main">7066 Nessus</span>

    7066 Nessus is a very red centaur on an eccentric orbit, located beyond Saturn in the outer Solar System. It was discovered on 26 April 1993, by astronomers of the Spacewatch program at the Kitt Peak National Observatory in Tucson, Arizona. The dark and reddish minor planet is likely elongated and measures approximately 60 kilometers in diameter. It was named after Nessus from Greek mythology.

    (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="nowrap">(208996) 2003 AZ<sub>84</sub></span> Plutino

    (208996) 2003 AZ84 (provisional designation 2003 AZ84) is a trans-Neptunian object with a possible moon located in the outer regions of the Solar System. It is approximately 940 kilometers across its longest axis, as it has an elongated shape. It belongs to the plutinos – a group of minor planets named after its largest member Pluto – as it orbits in a 2:3 resonance with Neptune in the Kuiper belt. It is the third-largest known plutino, after Pluto and Orcus. It was discovered on 13 January 2003, by American astronomers Chad Trujillo and Michael Brown during the NEAT survey using the Samuel Oschin telescope at Palomar Observatory.

    <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.

    (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.

    (79983) 1999 DF9 (provisional designation 1999 DF9) is a trans-Neptunian object of the Kuiper belt, classified as a non-resonant cubewano, that measures approximately 270 kilometers in diameter.

    (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">(612584) 2003 QX<sub>113</sub></span>

    (612584) 2003 QX113 is a large trans-Neptunian object from the scattered disc located in the outermost region of the Solar System. It is one of the most distant objects from the Sun at 60.5 AU. It was discovered by astronomers with the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories, Hawaii, when it was near aphelion on 31 August 2003. It was provisionally designated 2003 QX113.

    <span class="nowrap">(120216) 2004 EW<sub>95</sub></span>

    (120216) 2004 EW95, provisionally known as 2004 EW95, is a resonant trans-Neptunian object in the Kuiper belt located in the outermost regions of the Solar System. It measures approximately 291 kilometers in diameter. It has more carbon than typical of KBOs, and the first to be confirmed as having this composition in this region of space. It is thought to have originated closer to the Sun, perhaps even in the main asteroid belt.

    <span class="nowrap">(82075) 2000 YW<sub>134</sub></span>

    (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. As of 2021, neither the primary body nor its satellite have been named.

    (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.

    (469306) 1999 CD158 (provisional designation 1999 CD158) is a trans-Neptunian object from the circumstellar disc of the Kuiper belt, located in the outermost region of the Solar System. The relatively bright hot classical Kuiper belt object measures approximately 310 kilometers (190 miles) in diameter. It was discovered on 10 February 1999, by American astronomers Jane Luu, David Jewitt and Chad Trujillo at Mauna Kea Observatories on the Big Island of Hawaii, United States.

    (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.

    (589683) 2010 RF43 (provisional designation 2010 RF43) is a large trans-Neptunian object orbiting in the scattered disc in the outermost regions of the Solar System. The object was discovered on 9 September 2010, by American astronomers David Rabinowitz, Megan Schwamb and Suzanne Tourtellotte at ESO's La Silla Observatory in northern Chile.

    (445473) 2010 VZ98 (provisional designation 2010 VZ98) is a trans-Neptunian object of the scattered disc, orbiting the Sun in the outermost region of the Solar System. It has a diameter of approximately 400 kilometers.

    <span class="nowrap">2015 KH<sub>162</sub></span>

    2015 KH162 is a large trans-Neptunian object orbiting in the scattered disc region of the outermost Solar System. First observed in 2015, this minor planet is one of the most distant objects from the Sun at 60.6 AU, or twice as far as Neptune.

    <span class="nowrap">(127546) 2002 XU<sub>93</sub></span>

    (127546) 2002 XU93, provisional designation 2002 XU93, is a trans-Neptunian object and centaur on highly inclined and eccentric orbit in the outer region of the Solar System. It measures approximately 170 kilometers (110 mi) in diameter and is one of few objects with such an unusual orbit. It was discovered on 4 December 2002, by American astronomer Marc Buie at the Kitt Peak National Observatory in Arizona, United States.

    References

    1. 1 2 3 4 5 6 "15875 (1996 TP66)". Minor Planet Center. Retrieved 6 November 2018.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: 15875 (1996 TP66)" (2008-10-22 last obs.). Jet Propulsion Laboratory . Retrieved 6 November 2018.
    3. 1 2 Marc W. Buie. "Orbit Fit and Astrometric record for (15875)". Southwest Research Institute. Retrieved 6 November 2018.
    4. 1 2 3 4 5 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 6 November 2018.
    5. 1 2 3 4 5 Mommert, M.; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; et al. (May 2012). "TNOs are cool: A survey of the trans-Neptunian region. V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy and Astrophysics. 541: 17. arXiv: 1202.3657 . Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562. S2CID   119253817.
    6. 1 2 3 4 5 6 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.
    7. 1 2 "Asteroid (15875) 1996TP66 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site. Retrieved 6 November 2018.
    8. 1 2 Doressoundiram, A.; Peixinho, N.; Moullet, A.; Fornasier, S.; Barucci, M. A.; Beuzit, J.-L.; et al. (December 2007). "The Meudon Multicolor Survey (2MS) of Centaurs and Trans-Neptunian Objects: From Visible to Infrared Colors". The Astronomical Journal. 134 (6): 2186–2199. Bibcode:2007AJ....134.2186D. doi: 10.1086/522783 .
    9. 1 2 3 "LCDB Data for (15875)". Asteroid Lightcurve Database (LCDB). Retrieved 6 November 2018.
    10. 1 2 Romanishin, W.; Tegler, S. C. (March 1999). "Rotation rates of Kuiper-belt objects from their light curves". Nature . 398 (6723): 129–132. Bibcode:1999Natur.398..129R. doi:10.1038/18168. S2CID   4313184.
    11. ↑ "MPEC 1997-N03: 1996 TP66". Minor Planet Center. 2 July 1997. Retrieved 6 November 2018.
    12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 6 November 2018.
    13. ↑ Barkume, K. M.; Brown, M. E.; Schaller, E. L. (January 2008). "Near-Infrared Spectra of Centaurs and Kuiper Belt Objects". The Astronomical Journal. 135 (1): 55–67. Bibcode:2008AJ....135...55B. doi: 10.1088/0004-6256/135/1/55 .
    14. ↑ Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited". Astronomy and Astrophysics. 546: 20. arXiv: 1209.1896 . Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. S2CID   54776793.
    15. ↑ Hainaut, O. R.; Delsanti, A. C. (July 2002). "Colors of Minor Bodies in the Outer Solar System. A statistical analysis". Astronomy and Astrophysics. 389 (2): 641–664. Bibcode:2002A&A...389..641H. doi: 10.1051/0004-6361:20020431 .
    16. 1 2 "Asteroid (15875) 1996 TP66". Small Bodies Data Ferret. Retrieved 6 November 2018.
    17. ↑ Stansberry, J. A.; Cruikshank, D. P.; Grundy, W. G.; Margot, J. L.; Emery, J. P.; Fernandez, Y. R.; et al. (August 2005). "Albedos, Diameters (and a Density) of Kuiper Belt and Centaur Objects". American Astronomical Society. 37: 737. Bibcode:2005DPS....37.5205S.
    18. ↑ Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 6 November 2018.
    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.