2013 BL76

2013 BL76

The orbits of some of the most distant asteroids, 2013 BL76 at top left
Discovery[1][2]
Discovered by Mt. Lemmon Survey
Discovery date January 20, 2013
Designations
Trans-Neptunian object
Centaur[3]
Damocloid
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 1
Observation arc 687 days (1.88 yr)
Aphelion 2499 ±9.421 AU
~1920 AU[lower-alpha 1]
Perihelion 8.37058 AU (1.252221 Tm) (q)
1254 ±4.726 AU (a)
~964 AU[lower-alpha 1]
Eccentricity 0.99312 (e)
44,382 ±251 yr
~29900 yr[lower-alpha 1]
last perihelion: 2012-10-27
0.0272433° (M)
0.0000232226°/day (n)
Inclination 98.61911° (i)
180.20631° (Ω)
166.0668° (ω)
Known satellites none
Earth MOID 7.39224 AU (1.105863 Tm)
Jupiter MOID 3.51631 AU (526.032 Gm)
Saturn MOID 0.98692 AU (147.641 Gm)
Physical characteristics
Dimensions ~15–40 km[5]
30–40 km (assumed albedo 0.05-0.1)
21.6[6]
10.8[4][7]

    2013 BL76 is a minor planet (centaur)[3] from the scattered disk/Inner Oort cloud. Using an epoch of December 2014, it is the minor planet with the third-largest heliocentric semi-major axis in the Solar system (after 2005 VX3 and 2012 DR30).[8] 2013 BL76 has a barycentric semi-major axis of ~964 AU,[9][lower-alpha 1] which is also the third largest barycentric semi-major axis of any minor planet.

    With an absolute magnitude (H) of 10.8[7] and an unknown albedo, the object has an estimated diameter of 15–40 km.[5] Since it has not been seen out-gassing, it is not known if it is a comet or not. It might also be a damocloid, a type of minor planet that was originally a comet but lost most of its near-surface volatile materials after numerous orbits around the Sun. It also might be a dormant comet that simply has not been seen outgassing.

    2013 BL76 came to perihelion 8.3AU from the Sun on October 27, 2012, when it reached an apparent magnitude of about 20.[1] In 1927, when it was 100AU from the Sun, it had an apparent magnitude of about 30.8.[11] For comparison dwarf planet 90377 Sedna had an apparent magnitude of 21.7 when it was 100AU from the Sun.[12]

    It will not be 50 AU from the Sun until 2045. After leaving the planetary region of the Solar System, 2013 BL76 will have a barycentric aphelion of 1920 AU with an orbital period of 29900 years.[lower-alpha 1]

    In a 10 million year integration of the orbit, the nominal (best-fit) orbit remains 6.7AU (qmin) from the Sun, but one of the 3-sigma clones acquires a perihelion point of 0.5AU (inside the orbit of Venus).[3]

    2013 BL76 travels in a technically retrograde orbit around the Sun. It is actually orbiting in a plane nearly perpendicular to that of the ecliptic. It has the 55th highest inclination of any known asteroid, after 2010 GW147 and before 2014 HS150.

    Orbital evolution
    Epoch Barycentric
    Aphelion (Q)
    (AU)
    Orbital
    period
    yr
    1950 1849 28300
    2050 1920 29900

    Comparison

    2013 BL76 compared to some other very distant orbiting bodies. Including 90377 Sedna, 2015 DB216 (orbit wrong), 2000 OO67, 2004 VN112, 2005 VX3, 2006 SQ372, 2007 TG422, 2007 DA61, 2009 MS9, 2010 GB174, 2010 NV1, 2010 BK118, 2012 DR30, 2012 VP113, 2013 AZ60, 2013 RF98, 2015 ER61

    Largest semimajor axes of minor planets

    Minor planet designation Semi-major axis Semi-major axis
    (barycntr.)
    Perihelion Aphelion Aphelion
    (barycntr.)
    (H) Diameter (km) Orbital certainty (0–9)[lower-alpha 2] # obs. (arc in days)
    2002 GB32 213 206.7 35.3420 390 378 7.8
    (7.7)
    120 3 26(4733)
    (82158) 2001 FP185 220 216 34.2340 406 398 6.0 265 3 50(2461)
    2012 KA51 224 190 4.9 444 380 11.1 15 9 12(6)
    (148209) 2000 CR105 229.8 222.2 44.2000 415.5 400.4 6.3 320 3 54(3242)
    (468861) 2013 LU28 230 230 8.698 460 451.5 7.9 115 5 56(385)
    2006 UL321 261 257 23.5 498 490.5 7.6 125 9 3(1)
    2012 VP113 265 263.158 80.4500 448 445.88 4.0 460 5 26(739)
    1996 PW 267 240 2.5557 532 480 14.0 7 2 250(506)
    2011 OR17 (2010 KZ127) 272 270 3.0987 550 540 13.1 10 1 101(748)
    2013 RF98 320 316.7 36.288 603 597 8.6
    (8.64 ±0.34175)
    90 5 38(56)
    (336756) 2010 NV1 322.7 286 9.41587 635.9 562 10.6 34 1 147(1815)
    2004 VN112 328.8 327.3 47.3324 610.3 607.3 6.4 314 2 28(3611)
    (418993) 2009 MS9 349.55 352.5 11.00317 688.1 694 10.0
    (9.9)
    42 1 134(1995)
    2010 GB174 367 351.1 48.5600 686 653.7 6.5 223 3 18(965)
    2007 DA61 475 500 2.6550 950 900 15.1
    (14.913 ±0.470)
    4.5 4 78(29)
    2010 BK118 490 385 6.1050 980 770 10.2 38 1 292(1319)
    90377 Sedna 524.2 505.88 76.094 972.4 935.6 1.5 1000 2 90(8819)
    2007 TG422 530 501.8 35.5830 1030 968 6.2 343 2 34(1956)
    (87269) 2000 OO67 570 555 20.7900 1100 1110 9.2 60 2 34(2187)
    2002 RN109 720 850 2.7040 1440 1201 15.3 4 3 38(80)
    (308933) 2006 SQ372 765 792 24.172 1500 1585 8.1 110 2 65(1830)
    2013 AZ60 880 593 7.908 1700 1176 10.2 62.3 1 189(8067)
    2013 BL76 1251 940 8.37358 2494 1825 10.8 35 1 68(687)
    2012 DR30 (2009 FW54) 1300 1036 14.546 2600 2030 7.1 171 0 206(5375)
    2005 VX3 1300 1200 4.133 2700 2038 14.1 6 4 50(81)
    2014 FE72 2000 1500 36.3 4000 3000 6.0789 ± 0.1699 226 5 12(623)

    Notes

    1. 1 2 3 4 5 Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the semi-major axis and orbital period. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates.[10] Using JPL Horizons, the barycentric semi-major axis is approximately 964 AU.[9]
    2. 0–3 is high-certainty and well constrained, 9 is low-certainty and probably lost.

    References

    1. 1 2 "2013 BL76". Seicchi Yoshida's Home Page. Retrieved 2013-07-12.
    2. "MPEC 2013-C12 : 2013 BL76". IAU Minor Planet Center. 2013-02-03. Retrieved 2013-10-14. (K13B76L)
    3. 1 2 3 Marc W. Buie. "Orbit Fit and Astrometric record for 13BL76". SwRI (Space Science Department). Archived from the original on 2016-02-06. Retrieved 2016-02-03.
    4. 1 2 "JPL Small-Body Database Browser: (2013 BL76)" (last observation: 2014-08-25; arc: 1.88 years). Jet Propulsion Laboratory. Retrieved 25 March 2016.
    5. 1 2 "Absolute Magnitude (H)". NASA/JPL. Retrieved 2013-10-13.
    6. "AstDyS 2013BL76 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2016-02-04.
    7. 1 2 "2013 BL76". IAU minor planet center. Retrieved 2013-07-12.
    8. "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. Retrieved 2013-10-13. (Epoch defined at will change every 6 months or so)
    9. 1 2 Horizons output. "Barycentric Osculating Orbital Elements for 2013 BL76". Retrieved 2014-03-06. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
    10. Kaib, Nathan A.; Becker, Andrew C.; Jones, R. Lynne; Puckett, Andrew W.; Bizyaev, Dmitry; Dilday, Benjamin; Frieman, Joshua A.; Oravetz, Daniel J.; Pan, Kaike; Quinn, Thomas; Schneider, Donald P.; Watters, Shannon (2009). "2006 SQ372: A Likely Long-Period Comet from the Inner Oort Cloud". The Astrophysical Journal. 695 (1): 268–275. arXiv:0901.1690Freely accessible. Bibcode:2009ApJ...695..268K. doi:10.1088/0004-637X/695/1/268.
    11. "AstDys 2013BL76 Ephemerides for 1927 (when 100AU from Sun)". Department of Mathematics, University of Pisa, Italy. Retrieved 2013-10-14.
    12. "AstDys (90377) Sedna Ephemerides for 1975 (when 100AU from Sun)". Department of Mathematics, University of Pisa, Italy. Retrieved 2013-10-14.

    External links

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