(40314) 1999 KR16

Last updated

(40314) 1999 KR16
(40314) 1999 KR16 hst.jpg
Hubble Space Telescope image of 1999 KR16 taken in 2010
Discovery [1]
Discovered by A. Dalsanti
O. R. Hainaut
Discovery site La Silla Obs.
Discovery date16 May 1999
Designations
(40314) 1999 KR16
1999 KR16
TNO [2]  ·other [3]  · distant [1]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 2
Observation arc 16.09 yr (5,878 d)
Aphelion 64.604 AU
Perihelion 33.968 AU
49.286 AU
Eccentricity 0.3108
346.02 yr (126,383 d)
347.77°
0° 0m 10.08s / day
Inclination 24.771°
205.57°
≈ 26 February 2030 [4]
58.419°
Physical characteristics
254±37  km [5]
255 km(est.) [6]
5.8  h (half period?) [7]
11.7 h [8]
0.204±0.070 [5]
RR (very red) [9]
5.5 [1] [2]
5.527±0.039(R) [10]
5.7 [2]
5.59±0.02(R) [11]

    (40314) 1999 KR16 is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 kilometers (158 miles) in diameter. It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESO 's La Silla Observatory in northern Chile. [1] The very reddish object is a dwarf planet candidate and has a rotation period of 11.7 hours. [6] [12]

    Contents

    Orbit and classification

    The minor planet orbits the Sun at a distance of 34–65  AU once every 346 years (126,383 days; semi-major axis of 49.29 AU). Its orbit has an eccentricity of 0.31 and an inclination of 25° with respect to the ecliptic. [2]

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 26 May 2002. [13] As of 2019, it has not been named. [1]

    Physical characteristics

    1999 KR16 has two solutions of its rotation period of 6 and 12 hours, respectively, [7] [8] and an albedo of 0.20. [5]

    Related Research Articles

    A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has an orbital semi-major axis of 30.1 astronomical units (AU).

    8405 Asbolus is a centaur orbiting in the outer Solar System between the orbits of Jupiter and Neptune. It was discovered on 5 April 1995, by James Scotti and Robert Jedicke of Spacewatch (credited) at Kitt Peak Observatory in Arizona, United States. It is named after Asbolus, a centaur in Greek mythology and measures approximately 80 kilometers in diameter.

    <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 600 kilometers (400 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> Very red centaur on an eccentric orbit beyond Saturn in the outer Solar System

    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.

    <span class="mw-page-title-main">10370 Hylonome</span>

    10370 Hylonome (; prov. designation: 1995 DW2) is a minor planet orbiting in the outer Solar System. The dark and icy body belongs to the class of centaurs and measures approximately 72 kilometers (45 miles) in diameter. It was discovered on 27 February 1995, by English astronomer David C. Jewitt and Vietnamese American astronomer Jane Luu at the U.S. Mauna Kea Observatory in Hawaii, and later named after the mythological creature Hylonome.

    (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.

    <span class="nowrap">(84922) 2003 VS<sub>2</sub></span> Trans-Neptunian object

    (84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on 14 November 2003. Like Pluto, it is in a 2:3 orbital resonance with Neptune and is thus a plutino. Analysis of light-curve suggests that it is not a dwarf planet.

    <span class="nowrap">(15875) 1996 TP<sub>66</sub></span> Resonant trans-Neptunian object

    (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.

    (24835) 1995 SM55 (provisional designation 1995 SM55) is a trans-Neptunian object and member of the Haumea family that resides in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 19 September 1995, by American astronomer Nichole Danzl of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. It measures approximately 200 kilometers in diameter and was the second-brightest known object in the Kuiper belt, after Pluto, until 1996 TO66 was discovered.

    (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">(44594) 1999 OX<sub>3</sub></span>

    (44594) 1999 OX3 is an eccentric trans-Neptunian object with a centaur-like orbit from the outer Solar System, approximately 150 kilometers in diameter. It was discovered on 21 July 1999, by astronomers John Kavelaars, Brett Gladman, Matthew Holman and Jean-Marc Petit at Mauna Kea Observatories, Hawaii, United States.

    (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.

    (144897) 2004 UX10 (provisional designation 2004 UX10) is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi) and was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 20 October 2004 at Apache Point Observatory in Sunspot, New Mexico. The object is classified as a cubewano. It is near a 2:3 resonance with Neptune.

    (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.

    <span class="nowrap">(612095) 1999 OJ<sub>4</sub></span>

    (612095) 1999 OJ4 (provisional designation 1999 OJ4) is a trans-Neptunian object and binary system from the classical Kuiper belt, located in the outermost region of the Solar System. The bright cubewano belongs to the cold population and measures approximately 75 kilometers (47 miles) in diameter. It was first observed at Mauna Kea Observatory on 18 July 1999. Discovered in 2005, its minor-planet moon is just 3 kilometers smaller than its primary and has an orbital period of 84 days.

    <span class="nowrap">(82158) 2001 FP<sub>185</sub></span>

    (82158) 2001 FP185 (provisional designation 2001 FP185) is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States.

    <span class="nowrap">(416400) 2003 UZ<sub>117</sub></span>

    (416400) 2003 UZ117 (provisional designation 2003 UZ117) is a trans-Neptunian object and suspected member of the Haumea family, located in the Kuiper belt in the outermost region of the Solar System. It was discovered on 24 October 2003, by astronomers of the Spacewatch survey project at Kitt Peak Observatory, Arizona. The object may also be a non-resonant cubewano.

    References

    1. 1 2 3 4 5 "40314 (1999 KR16)". Minor Planet Center. Retrieved 11 September 2018.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: 40314 (1999 KR16)" (2015-06-19 last obs.). Jet Propulsion Laboratory . Retrieved 11 September 2018.
    3. ↑ Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 3 December 2018.
    4. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    5. 1 2 3 Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; Pal, A.; Müller, T. G.; Vilenius, E.; et al. (May 2012). ""TNOs are Cool": A survey of the trans-Neptunian region. IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS". Astronomy & Astrophysics. 541: 18. arXiv: 1202.1481 . Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. S2CID   118600525 . Retrieved 2 December 2015.
    6. 1 2 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 3 December 2018.
    7. 1 2 Thirouin, A.; Ortiz, J. L.; Campo Bagatin, A.; Pravec, P.; Morales, N.; Hainaut, O.; Duffard, R. (August 2012). "Short-term variability of 10 trans-Neptunian objects". Monthly Notices of the Royal Astronomical Society. 424 (4): 3156–3177. arXiv: 1207.2044 . Bibcode:2012MNRAS.424.3156T. doi: 10.1111/j.1365-2966.2012.21477.x . S2CID   53467482.
    8. 1 2 Sheppard, Scott S.; Jewitt, David C. (September 2002). "Time-resolved Photometry of Kuiper Belt Objects: Rotations, Shapes, and Phase Functions". The Astronomical Journal. 124 (3): 1757–1775. arXiv: astro-ph/0205392 . Bibcode:2002AJ....124.1757S. doi:10.1086/341954. S2CID   55644670 . Retrieved 2 December 2015.
    9. ↑ 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 . Retrieved 14 December 2016.
    10. ↑ Peixinho, N.; Delsanti, A.; Guilbert-Lepoutre, A.; Gafeira, R.; Lacerda, P. (October 2012). "The bimodal colors of Centaurs and small Kuiper belt objects". Astronomy and Astrophysics. 546: 12. arXiv: 1206.3153 . Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. S2CID   55876118 . Retrieved 14 December 2016.
    11. ↑ Jewitt, David; Peixinho, Nuno; Hsieh, Henry H. (November 2007). "U-Band Photometry of Kuiper Belt Objects". The Astronomical Journal. 134 (5): 2046–2053. Bibcode:2007AJ....134.2046J. doi: 10.1086/522787 .
    12. ↑ "LCDB Data for (40314)". Asteroid Lightcurve Database (LCDB). Retrieved 14 December 2016.
    13. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
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