(48639) 1995 TL8

Last updated

(48639) 1995 TL8
1995TL8-satellite-discovery.jpg
1995 TL8 and its satellite (unresolved) imaged by the Hubble Space Telescope
Discovery [1] [2]
Discovered by A. Gleason (Spacewatch)
Discovery site Kitt Peak National Obs.
Discovery date15 October 1995
Designations
(48639) 1995 TL8
1995 TL8
TNO [1]  ·Other TNO [3]
detached [4]  · distant [2]
Orbital characteristics [1]
Epoch 17 December 2020 (JD 2459200.5)
Uncertainty parameter 2
Observation arc 25.26 yr (9,225 days)
Aphelion 65.218 AU
Perihelion 39.937 AU
52.578 AU
Eccentricity 0.2404
381.25 yr (139,251 days)
46.972°
0° 0m 9.36s / day
Inclination 0.2499°
260.007°
84.397°
Known satellites 1 (D: 80 km) [5]
Physical characteristics
Dimensions 176 km [5]
420.27 km (calculated) [6]
495 km (estimated) [7]
0.07 (estimated) [7]
0.10 (assumed) [6]
0.369 [5]
RR [8]  · C (assumed) [6]
4.667±0.091(R) [9]  ·4.8 [1] [6]  ·5.1 [7]  ·5.290±0.060 [a]

    (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. [5]

    Contents

    Discovery

    1995 TL8 was discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak National Observatory, near Tucson, Arizona. [2]

    It was the first of the bodies presently classified as a scattered-disc object (SDO) [3] [ failed verification ] to be discovered, preceding the SDO prototype (15874) 1996 TL66 by almost a year. [10]

    Satellite

    Animation of two Hubble images of 1995 TL8's satellite in August 2001 1995TL8.gif
    Animation of two Hubble images of 1995 TL8's satellite in August 2001

    A companion was discovered by Denise C. Stephens and Keith S. Noll, from observations with the Hubble Space Telescope taken on 9 November 2002, and announced on 5 October 2005. The satellite, designated S/2002 (48639) 1, is relatively large, having a likely mass of about 10% of the primary. Its orbit has not been determined, but it was at a separation of only about 420 kilometres (260 mi) to the primary at the time of discovery, with a possible orbital period of about half a day and an estimated diameter of 161 kilometres (100 mi). [5]

    A relative size and distance comparison of the 1995 TL8 system with the Earth-Moon system. The scale of the Earth-Moon system has been reduced so Earth appears the same size as the 1995 TL8 primary. 1995 TL8 binary-earth comparison.jpg
    A relative size and distance comparison of the 1995 TL8 system with the Earth–Moon system. The scale of the Earth–Moon system has been reduced so Earth appears the same size as the 1995 TL8 primary.

    Scattered–extended object

    1995 TL8 is classified as detached object (scattered–extended) by the Deep Ecliptic Survey, since its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit. [4] However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity.

    Simulations made in 2007 show that 1995 TL8 appears to have less than a 1% chance of being in a 3:7 resonance with Neptune, but it does execute circulations near this resonance. [11]

    1995 TL8 AnimLong.gif
    1995TL8 Orbital Period.jpg
    Left: The near 3:7 resonance pattern of 1995 TL8 with Neptune only moves clockwise. It never halts and reverses course (i.e. librates).
    Right: The orbital period of 1995 TL8 missing the 7:3 (2.333) resonance of Neptune

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 20 November 2002. [12] As of 2018, it has not been named. [2]

    See also

    Notes

    1. ↑ Lellouch (2013): observations on 11 February 2011 gave an absolute magnitude of 5.290±0.060. Summary figures for (48639) at LCDB not found at ADS (2013A&A...557...60L)

    Related Research Articles

    (65407) 2002 RP120 (provisional designation 2002 RP120) is a trans-Neptunian object and damocloid from the outer Solar System. Its orbit is retrograde and comet-like, and has a high eccentricity. It was discovered on 4 September 2002 by astronomers with the LONEOS survey at Anderson Mesa Station, Arizona, in the United States. The unusual object measures approximately 14.6 kilometers (9.1 miles) in diameter and is likely elongated in shape. It is a slow rotator and potentially a tumbler as well. The object was probably ejected from the ecliptic by Neptune.

    (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">(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.

    <span class="nowrap">(42301) 2001 UR<sub>163</sub></span>

    (42301) 2001 UR163 (provisional designation 2001 UR163) is a resonant trans-Neptunian object and possible dwarf planet located in the outermost region of the Solar System. The object measures approximately 352 kilometers (220 miles) in diameter with a high albedo and stays in an uncommon orbital resonance (4:9) with Neptune. It was discovered on 21 October 2001 by astronomers of the Deep Ecliptic Survey program at Kitt Peak National Observatory near Tucson, Arizona, United States. As of 2021, it has not been named.

    (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.

    (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">(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.

    (523731) 2014 OK394 (provisional designation 1995 SN55) is a trans-Neptunian object that orbits in the outer Solar System beyond the orbit of Neptune. First observed as 1995 SN55 by Spacewatch on 20 September 1995, it was a lost minor planet with an insufficiently defined orbit with only 36 days of observations. On 8 October 2010, it was rediscovered by the Pan-STARRS 1 survey and later announced as 2014 OK394 in July 2016. It was not until November 2020 when amateur astronomers S. Deen and K. Ly identified 2014 OK394 and 1995 SN55 as the same object. This identification was confirmed and announced by the Minor Planet Center in January 2021.

    <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.

    (184212) 2004 PB112 (provisional designation 2004 PB112) is a trans-Neptunian object from the scattered disc, approximately 154 kilometers (96 miles) in diameter, and in a rare high-order orbital resonance ratio (4:27) with Neptune. It was discovered on 13 August 2004, by American astronomer Marc Buie at the Cerro Tololo Inter-American Observatory in Chile.

    (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.

    1999 TR11, is a resonant trans-Neptunian object from the Kuiper belt, located in the outermost region of the Solar System. The reddish plutino measures approximately 93 kilometers (58 miles) in diameter. It was first observed on 9 October 1999, by American astronomer Scott Sheppard at the Mauna Kea Observatories with the University of Hawaii's 2.2-meter telescope.

    <span class="nowrap">2015 RX<sub>245</sub></span>

    2015 RX245 is an extreme trans-Neptunian object, detached, on a highly eccentric orbit in the outermost region of the Solar System. It measures approximately 250 kilometers (160 miles) in diameter and is "possibly" a dwarf planet. It was first observed on 8 September 2015, by astronomers with Outer Solar System Origins Survey using the 3.6-meter Canada–France–Hawaii Telescope at Mauna Kea Observatories, Hawaii, in the United States.

    (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 490 kilometers (300 miles) in diameter. It was numbered in 2018 and remains unnamed.

    (501581) 2014 OB394, provisional designation 2014 OB394, is a trans-Neptunian object from the outermost region of the Solar System, approximately 260 kilometers (160 miles) in diameter. It was discovered on 25 August 2012, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The weak dwarf planet candidate was numbered in 2017 and remains without a name.

    (523706) 2014 HF200 (provisional designation 2014 HF200) is a trans-Neptunian object on an eccentric orbit from the scattered disc, located in the outermost region of the Solar System. It was discovered on 20 May 2012, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The dwarf planet candidate measures approximately 300 kilometers (190 miles) in diameter.

    (523683) 2014 CP23 (provisional designation 2014 CP23) is a trans-Neptunian object from the scattered disc located in the outermost region of the Solar System It was discovered on 29 October 2011, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. The dwarf planet candidate measures approximately 267 kilometers (170 miles) in diameter.

    (495603) 2015 AM281 (provisional designation 2015 AM281) is a resonant trans-Neptunian object in the outermost region of the Solar System, guesstimated at approximately 470 kilometers (290 miles) in diameter. It was discovered on 13 March 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States.

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 48639 (1995 TL8)" (2021-01-16 last obs.). Jet Propulsion Laboratory . Retrieved 14 March 2021.
    2. 1 2 3 4 "48639 (1995 TL8)". Minor Planet Center. Retrieved 16 November 2017.
    3. 1 2 Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 16 November 2017.
    4. 1 2 Marc W. Buie (22 October 2003). "Orbit Fit and Astrometric record for 48639". SwRI (Space Science Department). Retrieved 26 January 2009.
    5. 1 2 3 4 5 Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database – (48639) 1995 TL8". Johnston's Archive. Retrieved 16 November 2017.
    6. 1 2 3 4 "LCDB Data for (48639)". Asteroid Lightcurve Database (LCDB). Retrieved 16 November 2017.
    7. 1 2 3 Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 16 November 2017.
    8. ↑ 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 16 November 2016.
    9. ↑ 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 16 November 2017.
    10. ↑ "1996 TO66 -- ANOTHER LARGE TRANSNEPTUNIAN OBJECT". www.cbat.eps.harvard.edu. Retrieved 17 October 2024.
    11. ↑ 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. S2CID   122634598 . Retrieved 16 November 2017.
    12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 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.