(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
Dimensions222.59 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

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    <span class="nowrap">1998 WW<sub>31</sub></span>

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    <span class="nowrap">(48639) 1995 TL<sub>8</sub></span>

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

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

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    <span class="nowrap">(15875) 1996 TP<sub>66</sub></span>

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

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

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

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

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    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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