2013 FY27

2013 FY27
Discovery[1]
Discovered by Scott Sheppard
Chad Trujillo
(807)
Discovery date 17 March 2013
announced: 31 March 2014
Designations
MPC designation 2013 FY27
TNO, SDO[2]
Orbital characteristics[3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 7
Observation arc 1054 days (2.89 yr)
Aphelion 81.8481 AU (12.24430 Tm) (Q)
Perihelion 36.0577 AU (5.39416 Tm) (q)
58.9529 AU (8.81923 Tm) (a)
Eccentricity 0.38836 (e)
452.65 yr (165332 d)
209.4711° (M)
0° 0m 7.839s /day (n)
Inclination 32.9890° (i)
187.1719° (Ω)
139.623° (ω)
Earth MOID 35.111 AU (5.2525 Tm)
Jupiter MOID 31.4167 AU (4.69987 Tm)
Physical characteristics
Dimensions 752 km (Brown)[4]
530[lower-alpha 1]–1100[lower-alpha 2] km[3][5]
900 km[6]
0.1 to 0.4? (assumed range)
0.15 (theoretically expected value)[4]
22.1
3.0 (JPL/MPC)[3]
3.3 (Brown)[4]

    2013 FY27, also written 2013 FY27, is a trans-Neptunian object[3] that belongs to the scattered disc (like Eris).[6] Its discovery was announced on 31 March 2014.[1] It has an absolute magnitude (H) of 3.0,[3] which makes it very likely to be a dwarf planet.[4] Assuming an albedo of 0.15, it would be approximately 850 kilometres (530 mi) in diameter.[5] It is the ninth-intrinsically-brightest known trans-Neptunian object,[7] and is the largest unnumbered minor planet as of October 2015.

    2013 FY27 will come to perihelion around 2198,[lower-alpha 3] at a distance of about 36 AU.[3] It is currently near aphelion, 80 AU from the Sun, and, as a result, it has an apparent magnitude of 22.[1] Its orbit has a significant inclination of 33°.[3]

    First observed on 17 March 2013, it has an observation arc of about one year.[3] It came to opposition in early March 2014.

    The sednoid 2012 VP113 and the scattered-disc object 2013 FZ27 were discovered by the same survey as 2013 FY27 and were announced within about a week of one another.

    Most-distant known trans-Neptunian objects (TNOs)
    in the Solar System as of 26 February 2016[8]
    Object name Distance from the Sun (AU) Magnitude
    (vmag)
    Current Perihelion Aphelion
    V774104 103 N/A N/A 24
    Eris 96.3 37.8 97.6 18.7
    2007 OR10 87.5 33.0 100.8 21.7
    Sedna 85.7 76.0 939 21.0
    2014 FC69 84.2 40.3 106.9 24.1
    2006 QH181 83.4 37.8 96.7 23.6
    2012 VP113 83.3 80.5 438 23.4
    2013 FY27 80.3 36.1 81.8 22.1
    2010 GB174 70.8 48.7 693 25.1
    2000 CR105 60.5 44.3 412 23.9
    2008 ST291 59.9 42.4 154.5 22.2
    2003 QX113 59.9 36.7 62.1 22.5
    Including all known objects currently located at least twice as far as Neptune.[8]
    See List of trans-Neptunian objects for more.

    See also

    Notes

    1. ↑ Assuming an albedo of 0.4
    2. ↑ Assuming an albedo of 0.1
    3. ↑ The uncertainty in the year of perihelion passage is ≈56 years.[3]

    References

    1. 1 2 3 "MPEC 2014-F82 : 2013 FY27". IAU Minor Planet Center. 2014-03-31. Retrieved 2014-03-31. (K13F27Y)
    2. ↑ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2014-04-02.
    3. 1 2 3 4 5 6 7 8 9 "JPL Small-Body Database Browser: (2013 FY27)" (last observation: 2014-03-26; arc: 1.02 years). Jet Propulsion Laboratory. Retrieved 3 April 2016.
    4. 1 2 3 4 Mike Brown, How many dwarf planets are there in the outer solar system? (assumes H = 3.3)
    5. 1 2 Dan Bruton. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Department of Physics & Astronomy (Stephen F. Austin State University). Retrieved 2014-03-26.
    6. 1 2 Lakdawalla, Emily (2014-04-02). "More excitement in the outermost solar system: 2013 FY27, a new dwarf planet". Planetary Society blogs. The Planetary Society. Retrieved 2014-04-02. External link in |work= (help)
    7. ↑ "JPL Small-Body Database Search Engine: orbital class (TNO) and H < 3.1 (mag)". JPL Solar System Dynamics. Retrieved 2014-03-31.
    8. 1 2 "AstDyS-2, Asteroids - Dynamic Site". 2016-02-26. Retrieved 2016-02-29. Objects with distance from Sun over 59 AU

    External links

    This article is issued from Wikipedia - version of the Monday, April 04, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.