(202421) 2005 UQ513

Last updated
(202421) 2005 UQ513
2005uq513-20020822.gif
Precovery image of 2005 UQ513, taken by the Palomar Observatory in 22 August 2002. [1]
Discovery [2]
Discovered by M. E. Brown
D. L. Rabinowitz
C. A. Trujillo
Discovery date21 October 2005 [3]
Designations
(202421) 2005 UQ513
Cubewano (MPC) [4]
ScatExt (DES) [5]
Orbital characteristics [3] [6]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 8474 days (23.20 yr)
Earliest precovery date15 September 1990
Aphelion 49.689  AU (7.4334  Tm) (Q)
Perihelion 36.713 AU (5.4922 Tm) (q)
43.201 AU (6.4628 Tm) (a)
Eccentricity 0.15018 (e)
283.95 yr (103713 d)
223.93° (M)
0° 0m 12.496s / day (n)
Inclination 25.7315° (i)
307.8679° (Ω)
≈ 30 July 2123 [7]
±3 days
221.89° (ω)
Earth  MOID 35.763 AU (5.3501 Tm)
Jupiter  MOID 31.568 AU (4.7225 Tm)
TJupiter 5.253
Physical characteristics
Dimensions498+63
−75 km [8]
7.03  h (0.293  d)
7.03 hr? [3]
0.31+0.12
−0.065 [8]
20.8 [9]
3.97 [3]

    (202421) 2005 UQ513 (provisional designation 2005 UQ513) is a cubewano with an absolute magnitude of 3.97. [3] Its spectrum has a weak signature of absorption by water ice. [10] [11] Like Quaoar, it has a very red spectrum, [12] [13] which indicates that its surface probably contains many complex, processed organic molecules. [12] Its light curve shows variations of Δm=0.3 mag, but no period has been determined. [13]

    Contents

    Classification

    2005 UQ513 has a perihelion of 37.3 AU. [3] The Minor Planet Center (MPC) classifies it as a cubewano [4] while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended). [5] Although dynamically it would have been a good candidate to be a member of the Haumea collisional family, given its red spectrum, it is not. [12] [13]

    Distance

    As of December 2018, it is currently 48.0 AU from the Sun. [9] It will come to perihelion in 2123. [7]

    It has been observed 194 times over 14 oppositions with precovery images back to 1990. [3]

    See also

    Related Research Articles

    <span class="mw-page-title-main">Classical Kuiper belt object</span> Kuiper belt object, not controlled by an orbital resonance with Neptune

    A classical Kuiper belt object, also called a cubewano ( "QB1-o"), is a low-eccentricity Kuiper belt object (KBO) that orbits beyond Neptune and is not controlled by an orbital resonance with Neptune. Cubewanos have orbits with semi-major axes in the 40–50 AU range and, unlike Pluto, do not cross Neptune's orbit. That is, they have low-eccentricity and sometimes low-inclination orbits like the classical planets.

    <span class="mw-page-title-main">Haumea</span> Dwarf planet in the Solar System

    Haumea is a dwarf planet located beyond Neptune's orbit. It was discovered in 2004 by a team headed by Mike Brown of Caltech at the Palomar Observatory in the United States and disputably also in 2005 by a team headed by José Luis Ortiz Moreno at the Sierra Nevada Observatory in Spain. On September 17, 2008, it was named after Haumea, the Hawaiian goddess of childbirth, under the expectation by the International Astronomical Union (IAU) that it would prove to be a dwarf planet. Nominal estimates make it the third-largest known trans-Neptunian object, after Eris and Pluto, and approximately the size of Uranus's moon Titania.

    <span class="mw-page-title-main">Makemake</span> Dwarf planet in the Outer Solar System

    Makemake is a dwarf planet and the second-largest of what are known as the classical population of Kuiper belt objects, with a diameter approximately that of Saturn's moon Iapetus, or 60% that of Pluto. It has one known satellite. Its extremely low average temperature, about 40 K (−230 °C), means its surface is covered with methane, ethane, and possibly nitrogen ices.

    <span class="nowrap">(19308) 1996 TO<sub>66</sub></span> Trans-Neptunian object in the Kuiper belt

    (19308) 1996 TO66 (provisional designation 1996 TO66) is a trans-Neptunian object that was discovered in 1996 by Chadwick Trujillo, David Jewitt and Jane Luu. Until 20000 Varuna was discovered, it was the second-largest known object in the Kuiper belt, after Pluto.

    <span class="nowrap">(90568) 2004 GV<sub>9</sub></span>

    (90568) 2004 GV9 (provisional designation 2004 GV9) is a trans-Neptunian object that was discovered on April 13, 2004 by NEAT. It has been listed as a cubewano by the Minor Planet Center. It was discovered on 13 April 2004 by NEAT. It has been observed forty-seven times, with precovery images back to 1954. The object has an orbital period of 273.88 years. Its maximum possible distance from the Sun (aphelion) is 45.62 AU, and its closest (perihelion) is 38.7 AU, and currently 39.7 AU from the sun. It has an inclination of 21.9718, and eccentricity of 0.082.

    <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="nowrap">(55637) 2002 UX<sub>25</sub></span> Spitzer dwarf-planet candidate

    (55637) 2002 UX25 (provisional designation 2002 UX25) is a trans-Neptunian object that orbits the Sun in the Kuiper belt beyond Neptune. It briefly garnered scientific attention when it was found to have an unexpectedly low density of about 0.82 g/cm3.

    <span class="nowrap">(55636) 2002 TX<sub>300</sub></span> Kuiper Belt object

    (55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) program.

    54598 Bienor is a centaur that grazes the orbit of Uranus. It is named after the mythological centaur Bienor. Its closest approach to the Sun (perihelion) is 13.2 AU. As of 2020, Bienor is 14.2 AU from the Sun and will reach perihelion in January 2028. It measured approximately 198 kilometers in diameter.

    <span class="nowrap">(145452) 2005 RN<sub>43</sub></span> Classical Kuiper belt object

    (145452) 2005 RN43 (provisional designation 2005 RN43) is a classical Kuiper belt object. It has an estimated diameter of 679+55
    −73     km    . It was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 10 September 2005 at Apache Point Observatory in Sunspot, New Mexico. Brown estimates that it is possibly a dwarf planet.

    <span class="mw-page-title-main">79360 Sila–Nunam</span>

    79360 Sila–Nunam, provisional designation 1997 CS29, is a cold classical Kuiper belt object (cubewano) and binary system made up of components of almost equal size, called Sila and Nunam, orbiting beyond Neptune in the Solar System. The name of the system is the combined names of the two bodies, Sila and Nunam.

    (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.

    <span class="nowrap">(120178) 2003 OP<sub>32</sub></span>

    (120178) 2003 OP32, also written as (120178) 2003 OP32, is a trans-Neptunian object (TNO) that resides in the Kuiper belt. It was discovered on July 26, 2003 by Michael E. Brown, Chad Trujillo and David L. Rabinowitz at Palomar Mountain in California.

    <span class="nowrap">(145453) 2005 RR<sub>43</sub></span>

    (145453) 2005 RR43 (provisional designation 2005 RR43) is a trans-Neptunian object (TNO) estimated to be about 250 km in diameter. It was discovered on 9 September 2005 by Andrew Becker, Andrew Puckett and Jeremy Kubica at Apache Point Observatory in Sunspot, New Mexico.

    <span class="nowrap">(455502) 2003 UZ<sub>413</sub></span>

    (455502) 2003 UZ413 (provisional designation 2003 UZ413) is a trans-Neptunian object (TNO) with an absolute magnitude of 4.38. It is in a 2:3 orbital resonance with Neptune, thus it is classified as a plutino. There are indications it may be dense enough to be a dwarf planet. It was given the minor planet number 455502 on 22 February 2016.

    <span class="nowrap">(308193) 2005 CB<sub>79</sub></span>

    (308193) 2005 CB79 is a trans-Neptunian object that is a member of the Haumea family.

    <span class="nowrap">(612533) 2002 XV<sub>93</sub></span>

    (612533) 2002 XV93 (provisional designation 2002 XV93) is a trans-Neptunian object (TNO) with an absolute magnitude of 5.4. A 2:3 orbital resonance with Neptune makes it a plutino.

    (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">(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.

    (523635) 2010 DN93 (provisional designation 2010 DN93) is a trans-Neptunian object from in the scattered disc located in the outermost region of the Solar System. It was discovered on 26 February 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. Assuming a low albedo, the object is estimated at approximately 490 kilometers (300 miles) in diameter. It was numbered in 2018 and remains unnamed.

    References

    1. ↑ Lowe, Andrew. "(202421) 2005 UQ513 Precovery Images". andrew-lowe.ca.
    2. ↑ Brown, M.; Trujillo, C.; Rabinowitz, D.; Marsden, B. G. (2007). "2003 UY413, 2003 UZ413, 2004 NT33, 2005 CA79, 2005 CB79, 2005 UQ513". Minor Planet Electronic Circulars. 2007-R02: R02. Bibcode:2007MPEC....R...02B.
    3. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: (2005 UQ513)" (2011-12-26 last obs., 12 opp). Retrieved 7 April 2016.
    4. 1 2 "MPEC 2010-S44 : DISTANT MINOR PLANETS (2010 OCT. 11.0 TT)". IAU Minor Planet Center. 2010-09-25. Retrieved 2011-01-26.
    5. 1 2 Marc W. Buie. "Orbit Fit and Astrometric record for 202421" (2012/05/06 using 59 observations). SwRI (Space Science Department). Retrieved 2012-05-05.
    6. ↑ "AstDyS (202421) 2005UQ513 Orbital information". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
    7. 1 2 JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    8. 1 2 TNOs are Cool: A survey of the trans-Neptunian region. X. Analysis of classical Kuiper belt objects from Herschel* and Spitzer observations p. 18 arXiv:1403.6309
    9. 1 2 "AstDyS (202421) 2005UQ513 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
    10. ↑ Ragozzine, D. & Brown, M. E. (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". The Astronomical Journal. 134 (6): 2160–2167. arXiv: 0709.0328 . Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID   8387493 . Retrieved 2009-12-05.
    11. ↑ Trujillo, C. A., Sheppard, S. S., & Schaller E. L. (2011). A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects arXiv : 1102.1971
    12. 1 2 3 Pinilla-Alonso, N., Licandro, J., & Lorenzi, V. (2008). Visible spectroscopy in the neighborhood of 2003 EL61 (Haumea) arXiv : 0807.2670
    13. 1 2 3 Snodgrass, C., Carry, B., Dumas, C., & Hainaut, O. (2009). Characterisation of candidate members of (136108) Haumea’s family arXiv : 0912.3171
    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.