(55565) 2002 AW197

(55565) 2002 AW197

Probable dwarf planet 2002 AW197 as taken by the Spitzer Space Telescope on 13 April 2004
Discovery[1]
Discovered by Michael E. Brown
Chad Trujillo
Eleanor F. Helin
Michael Hicks
Kenneth J. Lawrence
Steven H. Pravdo
Palomar Observatory (675)
Discovery date 10 January 2002
Designations
MPC designation (55565) 2002 AW197
none
Cubewano (MPC)[2]
Extended (DES)[3]
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 6647 days (18.20 yr)
Aphelion 53.771 AU (8.0440 Tm)
Perihelion 41.282 AU (6.1757 Tm)
47.526 AU (7.1098 Tm)
Eccentricity 0.13139
327.65 yr (119674 d)
4.31 km/s
293.876°
0° 0m 10.83s / day
Inclination 24.351°
297.438°
293.300°
Earth MOID 40.3467 AU (6.03578 Tm)
Jupiter MOID 36.369 AU (5.4407 Tm)
Physical characteristics
Dimensions

768+39
−38 km [5]

734+116
−108 km[6]
700±50 km[7]
8.86 h (0.369 d)
8.86 h [4]
0.117+0.04
−0.03[6]
0.17±0.03 [7]
Temperature ≈ 39–40 K
(moderately red)
B−V=0.91, V−R=0.56[8]
20.0 (opposition)[9][10]
3.5[4]

    (55565) 2002 AW197 is a classical Kuiper belt object (cubewano). Measurements with the Spitzer Space Telescope have confirmed 2002 AW197 as a probable dwarf planet, although it has not been officially classified as such by the IAU. Light-curve-amplitude analysis shows only small deviations, which suggests that 2002 AW197 is a spheroid with small albedo spots.[11] Tancredi (2010) accepts it as a dwarf planet.[12] Mike Brown's website lists it as a highly likely dwarf planet.[13]

    It was discovered on January 10, 2002, by Michael Brown et al.[1] It is located near the Kuiper cliff.

    Characteristics

    Observations of thermal emissions by the Spitzer Space Telescope in 2007 give a diameter of 734+116
    −108     km    [6] and an albedo of 0.117+0.04
    −0.03    .[6] The newest estimate is 768+39
    −38     km    [5]

    Surface

    ESO analysis of spectra reveals a strong red slope and no presence of water ice[14] (in contrast to Quaoar, also red) suggesting organic material (see comparison of colours and typical composition inferred from spectra of the TNOs).

    Distance

    As of 2013, it is currently 46.0 AU from the Sun.[9] It will come to perihelion around 2078.[4]

    References

    1. 1 2 Marsden, Brian G. (2002-07-20). "MPEC 2002-O30 : 2002 AW197". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 2010-01-06.
    2. ↑ "MPEC 2009-R09 :Distant Minor Planets (2009 SEPT. 16.0 TT)". IAU Minor Planet Center. 2009-09-04. Retrieved 2009-10-04.
    3. ↑ Marc W. Buie. "Orbit Fit and Astrometric record for 55565" (2009-03-23 using 112 observations). SwRI (Space Science Department). Retrieved 2009-10-04.
    4. 1 2 3 4 "JPL Small-Body Database Browser: 55565 (2002 AW197)" (2005-01-16 last obs). Retrieved 6 April 2016.
    5. 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
    6. 1 2 3 4 John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; John Spencer; David Trilling; et al. (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538Freely accessible [astro-ph].
    7. 1 2 Cruikshank, Dale P.; Stansberry, John A.; Emery, Joshua P.; et al. (2005). "The High-Albedo Kuiper Belt Object (55565) 2002 AW197". The Astrophysical Journal. 624 (1): L53–L56. Bibcode:2005ApJ...624L..53C. doi:10.1086/430420.
    8. ↑ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Retrieved 2009-12-30.
    9. 1 2 "AstDys (55565) 2002AW197 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2013-12-14.
    10. ↑ "HORIZONS Web-Interface". JPL Solar System Dynamics. Retrieved 2008-07-02.
    11. ↑ Tancredi, G., & Favre, S. (2008) Which are the dwarfs in the Solar System?. Depto. Astronomía, Fac. Ciencias, Montevideo, Uruguay; Observatorio Astronómico Los Molinos, MEC, Uruguay. Retrieved 10-08-2011
    12. ↑ Tancredi, G. (2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009.
    13. ↑ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 31 August 2016.
    14. ↑ D. Ragozzine; M. E. Brown (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328Freely accessible. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. Retrieved 2009-12-05.

    Further

    External links

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