(307261) 2002 MS4

(307261) 2002 MS4
Discovery[1]
Discovered by Chad Trujillo,
Michael E. Brown
Discovery date 18 June 2002
Designations
MPC designation 2002 MS4
none
Cubewano (MPC)[2]
ScatExt (DES)[3]
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 20569 days (56.31 yr)
Aphelion 47.740 AU (7.1418 Tm)
Perihelion 35.694 AU (5.3397 Tm)
41.717 AU (6.2408 Tm)
Eccentricity 0.14439
269.45 yr (98415.8 d)
4.58 km/s
216.187°
0° 0m 13.168s / day
Inclination 17.677°
215.963°
215.534°
Earth MOID 34.7228 AU (5.19446 Tm)
Jupiter MOID 30.7148 AU (4.59487 Tm)
Jupiter Tisserand parameter 5.464
Physical characteristics
Dimensions 934±47 km[5]
0.051+0.036
−0.022 [5]
Temperature ≈ 43 K
B−V=0.69;
V−R=0.38 [6]
20.6[7]
3.7[4]
3.5±0.4 (R-band)[5]

    (307261) 2002 MS4 is a large classical Kuiper belt object,[2] the second-largest known object in the Solar System without a name, after 2007 OR10. It was discovered in 2002 by Chad Trujillo and Michael Brown.

    Brown's website lists it as nearly certain to be a dwarf planet.[8] The Spitzer Space Telescope estimated it to have a diameter of 726±123 km.[9] The Herschel team estimates it to be 934±47 km, which would make it one of the 10 largest TNOs currently known[5] and large enough to be considered a dwarf planet under the 2006 draft proposal of the IAU.[10] It is currently 47.2 AU from the Sun[7] and will come to perihelion in 2123.[4]

    It has been observed 55 times, with precovery images back to 1954.[4]

    References

    1. ↑ "MPEC 2002-W27 : 2002 MS4, 2002 QX47, 2002 VR128". IAU Minor Planet Center. 2002-11-21. Retrieved 2009-08-26.
    2. 1 2 "MPEC 2009-P26 :Distant Minor Planets (2009 AUG. 17.0 TT)". IAU Minor Planet Center. 2009-08-07. Retrieved 2009-08-31.
    3. ↑ Marc W. Buie (2008-05-03). "Orbit Fit and Astrometric record for 02MS4". SwRI (Space Science Department). Archived from the original on 29 June 2011. Retrieved 2009-08-31.
    4. 1 2 3 4 "JPL Small-Body Database Browser: 307261 (2002 MS4)" (2009-09-19 last obs.). Jet Propulsion Laboratory. Retrieved 7 April 2016.
    5. 1 2 3 4 Vilenius, E.; Kiss, C.; Mommert, M.; et al. (2012). ""TNOs are Cool": A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects". Astronomy & Astrophysics. 541: A94. arXiv:1204.0697Freely accessible. Bibcode:2012A&A...541A..94V. doi:10.1051/0004-6361/201118743.
    6. ↑ Tegler, Stephen C. (2006-01-26). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on November 16, 2007. Retrieved 2006-11-05.
    7. 1 2 "AstDyS 2002MS4 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 2009-09-04. Retrieved 2009-08-27.
    8. ↑ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2011-10-18. Retrieved 2011-08-25.
    9. ↑ Stansberry, Grundy, Brown, Spencer, Trilling, Cruikshank, Luc Margot Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope (2007) Preprint arXiv
    10. ↑ O. Gingerich (2006). "The Path to Defining Planets" (PDF). Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair. Retrieved 2007-03-13.

    External links

    This article is issued from Wikipedia - version of the 9/8/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.