(82158) 2001 FP185

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(82158) 2001 FP185
E trokhia tou (82158) 2001 FP185.gif
Discovery [1] [2]
Discovered by M. W. Buie
Discovery site Kitt Peak National Obs.
Discovery date26 March 2001
Designations
(82158) 2001 FP185
2001 FP185
TNO [1]  · SDO [3]  · distant [2]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 2
Observation arc 16.25 yr (5,937 days)
Aphelion 420.18 AU
Perihelion 34.280 AU
227.23 AU
Eccentricity 0.8491
3425.31 yr (1,251,096 days)
1.4289°
0° 0m 1.08s / day
Inclination 30.763°
179.31°
7.1638°
Physical characteristics
Dimensions 222.59 km (derived) [4]
332±31 km [3] [5]
336 km (radiometric) [6]
0.046±0.007 [5]
0.05 (radiometric) [6]
0.10 (assumed) [4]
IR [3] [7]  · C [4]
B–R = 1.38 [3]
B–V = 0.860±0.040 [8]  ·0.820±0.048 [9]  ·0.820±0.020 [7]
V–R = 0.520±0.040 [8]  ·0.572±0.038 [9]  ·0.580±0.020 [7]
V–I = 1.070±0.060 [8]  ·1.013±0.072 [9]  ·1.060±0.010 [7]
5.94±0.03(R) [8]  ·5.940±0.053(R) [10]  ·6.2 [1]  ·6.38 [4] [11]  ·6.4 [6]

    (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. [2]

    Contents

    Orbit and classification

    2001 FP185 is a scattered-disc object which belong to the most distant and coldest objects in the Solar System and are thought to be source of most periodic comets.

    It orbits the Sun at a distance of 34.3–420.2  AU once every 3425 years and 4 months (1,251,096 days). Its orbit has an eccentricity of 0.85 and an inclination of 31° with respect to the ecliptic. [1] A first precovery was taken by the Sloan Digital Sky Survey in March 1999, extending the body's observation arc by 2 years prior to its official discovery observation at Kitt Peak. [2]

    Planet Nine co-orbital

    If a massive trans-Neptunian object exists, like hypothetical Planet Nine , 2001 FP185 may be co-orbital with it. [12] [13]

    Physical characteristics

    Spectra and colors

    2001 FP185's color has extensively been measured. [7] [8] [9] The object has a determined BR and IR spectra, which are intermediate classes of the very blue BB and very red RR spectra. [3] [7]

    Diameter and albedo

    According to astronomer Michael Brown and based on radiometric observations, 2001 FP185 measures 336 kilometers in diameter and its surface has an (assumed) albedo of 0.05. [6] Observations with the PACS-instrument of the Herschel Space Observatory during a survey of scattered-disc objects ("TNO are cool") found a similar diameter of 332 kilometer with an albedo of 0.046. [5] The Collaborative Asteroid Lightcurve Link assumes a higher albedo of 0.10 and consequently derives a much shorter diameter of 222 kilometers based on an absolute magnitude of 6.38. [4] Brown considers 2001 FP185 to be possibly a dwarf planet (see list). [6]

    Lightcurve

    No rotational lightcurve of 2001 FP185 has been obtained from photometric observations. The body's rotation period, pole axis and brightness amplitude remains unknown. [4]

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 4 May 2004. [14] As of 2018, it has not been named. [2]

    See also

    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).

    5145 Pholus is an eccentric centaur in the outer Solar System, approximately 180 kilometers in diameter, that crosses the orbit of both Saturn and Neptune. It was discovered on 9 January 1992 by American astronomer David Rabinowitz (uncredited) of UA's Spacewatch survey at the Kitt Peak National Observatory in Arizona, United States. The very reddish object has an elongated shape and a rotation period of 9.98 hours. It was named after the centaur Pholus from Greek mythology.

    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="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.

    <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.

    <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">(40314) 1999 KR<sub>16</sub></span>

    (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. The very reddish object is a dwarf planet candidate and has a rotation period of 11.7 hours.

    83982 Crantor (provisional designation 2002 GO9) is a centaur in a 1:1 resonance with Uranus, approximately 60 kilometers (37 miles) in diameter. It was discovered on 12 April 2002, by astronomers of the Near-Earth Asteroid Tracking at the Palomar Observatory in California, United States. This minor planet was named for Crantor from Greek mythology.

    <span class="mw-page-title-main">31824 Elatus</span> Centaur

    31824 Elatus (; provisional designation 1999 UG5) is a very red centaur from the outer Solar System, approximately 48 kilometers (30 miles) in diameter. It was discovered on 29 October 1999, by astronomers of the Catalina Sky Survey at Mount Lemmon Observatory in Arizona, United States. The minor planet was named after Elatus, a centaur from Greek mythology.

    <span class="mw-page-title-main">32532 Thereus</span>

    32532 Thereus (; provisional designation 2001 PT13) is a centaur from the outer Solar System, approximately 80 kilometers (50 miles) in diameter. It was discovered on 9 August 2001, by astronomers of the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This minor planet was named for the phrase thēreios bia 'beastly strength', used to describe centaurs in Greek mythology.

    <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.

    (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.

    (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.

    (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.

    2011 MM4, provisional designation: 2011 MM4, is a sizable centaur and retrograde damocloid from the outer Solar System, approximately 64 kilometers (40 miles) in diameter. It was discovered on 24 June 2011, by astronomers with the Pan-STARRS 1 at the Haleakala Obs. in Hawaii.

    References

    1. 1 2 3 4 5 "JPL Small-Body Database Browser: 82158 (2001 FP185)" (2015-06-22 last obs.). Jet Propulsion Laboratory . Retrieved 2 August 2017.
    2. 1 2 3 4 5 "82158 (2001 FP185)". Minor Planet Center. Retrieved 2 August 2017.
    3. 1 2 3 4 5 "List of Known Trans-Neptunian Objects". Johnston's Archive. 22 July 2017. Retrieved 2 August 2017.
    4. 1 2 3 4 5 6 "LCDB Data for (82158)". Asteroid Lightcurve Database (LCDB). Retrieved 2 August 2017.
    5. 1 2 3 Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; Pal, A.; Müller, T. G.; 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 and Astrophysics. 541: 18. arXiv: 1202.1481 . Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. S2CID   118600525.
    6. 1 2 3 4 5 "How many dwarf planets are there in the outer solar system?". Mike Brown. Retrieved 2 August 2017.
    7. 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.
    8. 1 2 3 4 5 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 .
    9. 1 2 3 4 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.
    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.
    11. ↑ Romanishin, W.; Tegler, S. C. (December 2005). "Accurate absolute magnitudes for Kuiper belt objects and Centaurs". Icarus. 179 (2): 523–526. Bibcode:2005Icar..179..523R. doi:10.1016/j.icarus.2005.06.016.
    12. ↑ de la Fuente Marcos, C.; de la Fuente Marcos, R. (September 2014). "Extreme trans-Neptunian objects and the Kozai mechanism: signalling the presence of trans-Plutonian planets". Monthly Notices of the Royal Astronomical Society: Letters. 443 (1): L59–L63. arXiv: 1406.0715 . Bibcode:2014MNRAS.443L..59D. doi: 10.1093/mnrasl/slu084 . S2CID   118622180.
    13. ↑ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raú; l; Aarseth, Sverre J. (January 2015). "Flipping minor bodies: what comet 96P/Machholz 1 can tell us about the orbital evolution of extreme trans-Neptunian objects and the production of near-Earth objects on retrograde orbits". Monthly Notices of the Royal Astronomical Society. 446 (2): 1867–1873. arXiv: 1410.6307 . Bibcode:2015MNRAS.446.1867D. doi: 10.1093/mnras/stu2230 . S2CID   119256764.
    14. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
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