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C/2015 ER61 (PanSTARRS)

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(Redirected from 2015 ER61) Comet, inner Oort cloud object

C/2015 ER61 (PanSTARRS)
Discovery
Discovered byPan-STARRS 1 (F51)
Discovery date15 March 2015
Orbital characteristics
Epoch7 May 2017 (JD 2457880.5)
Observation arc1.96 yr
Aphelion
  • 2456±62 AU
  • 1425/854 AU
Perihelion1.0421 AU
Semi-major axis
  • 1229±31 AU
  • 715/428 AU
Eccentricity0.99730
Orbital period
  • 7591 years
  • 9000 years (epoch 2050)
Inclination6.3490°
Longitude of
ascending node		235.21°
Argument of
periapsis		68.197°
Earth MOID0.1016 AU
Mars MOID<0.00005 AU
Jupiter MOID0.0794 AU
Saturn MOID0.2869 AU
Physical characteristics
Dimensions
  • 8–20 km
  • 20 km
Geometric albedo~0.05 (assumed)
Comet total
magnitude (M1)
  • 20.5 (January 2016)
  • 14.74 (peak 1 May 2017)

C/2015 ER61 (PanSTARRS) is a comet and inner Oort cloud object. When classified as a minor planet, it had the fourth-largest aphelion of any known minor planet in the Solar System, after 2005 VX3, 2012 DR30, and 2013 BL76. It additionally had the most eccentric orbit of any known minor planet, with its distance from the Sun varying by about 99.9% during the course of its orbit, followed by 2005 VX3 with an eccentricity of 0.9973. On 30 January 2016, it was classified as a comet when it was 5.7 AU from the Sun. It comes close to Jupiter, and a close approach in the past threw it on the distant orbit it is on now.

Though the comet nucleus was probably mildly active, early asteroidal estimates gave an absolute magnitude (H) of 12.3, which would suggest a nucleus as large as 8–20 km in diameter. But it could easily be half that size due to activity brightening the nucleus.

2017 perihelion

C/2015 ER61 was discovered on 15 March 2015 when it was 8.44 AU from the Sun, and magnitude 21.5. By early February 2016, the object reached magnitude 20, and made a close approach to Jupiter on 28 March 2016 of 0.9245 AU. This changed its orbit, significantly decreasing its aphelion distance from 1430 AU to ~1200 AU, and as it passed through the inner Solar System its aphelion decreased to 770 AU, and by 2020 it had an aphelion of 854 AU.

The barycentric orbital period will decrease from 19000 years (epoch 1950) to 9000 years (epoch 2050).

As of January 2017, it was magnitude 13, and increasing in brightness. On 4 April 2017, it was detected outbursting to magnitude 6.5. On 19 April 2017, it reached its closest point to Earth of ~1.2 AU. At this point, it was about apparent magnitude 8, and, assuming a size of 20 km, have an apparent size of 19 mas. It came to perihelion (closest approach to the Sun) on 10 May 2017. It will not be 50 AU from the Sun until 2045.

Orbital elements table

Dist.
from
Sun 		Event Epoch Aphelion
(Q) 		Perihelion
(q) 		Semi-major axis
(a) 		Eccentricity
(e) 		Period
(p) 		Inclination
(i) 		Longitude ascending node
(Ω) 		Mean anomaly
(M) 		Argument of perihelion
(ω)
(AU) (AU) (years) (°)
36.5 2000-01-01 1423.4 1.05378 712.2 0.99852 18,990 6.12745 239.06 359.671 63.99
20.2 2010-01-01 1435.4 1.05377 718.2 0.99853 19,240 6.12732 239.03 359.862 64.01
9.01 2015-01-01 1430.8 1.05347 715.9 0.99853 19,140 6.12819 238.97 359.956 64.08
8.44 discovery 2015-03-15 1436.1 1.05313 718.6 0.99853 19,250 6.12879 238.95 359.960 64.11
6.00 2016-01-01 1667.3 1.04763 834.2 0.99874 24,080 6.15827 238.25 359.980 64.92
5.204 Jupiter approach 2016-03-28 1291.9 1.04030 646.5 0.99839 16,420 6.24250 236.73 359.976 66.64
2.242 2017-01-01 324.6 1.03505 162.8 0.99364 2,080 6.34928 235.27 359.939 68.46
1.079 Earth approach 2017-04-04 164.3 1.03830 82.7 0.98744 750 6.34595 235.27 359.953 68.30
1.0397 Perihelion 2017-05-10 210.0 1.03973 105.5 0.99015 1,080 6.34423 235.25 0.0004 67.92
3.437 2018-01-01 1091.1 1.04449 546.1 0.99809 12,750 6.34438 235.23 0.018 68.27
9.78 2020-01-01 857.8 1.04583 429.4 0.99756 8,890 6.34009 235.21 0.107 68.29
56.03 2050-01-01 854.6 1.04649 427.8 0.99755 8,840 6.33543 235.18 1.329 68.34

Comparison

Sedna compared to some other very distant orbiting bodies including 2015 DB216 (orbit wrong), 2000 OO67, 474640 Alicanto, 2005 VX3, 2006 SQ372, 2007 TG422, 2007 DA61, 2009 MS9, 2010 GB174, 2010 NV1, 2010 BK118, 2012 DR30, 2012 VP113, 2013 BL76, 2013 AZ60, 2013 RF98, 2015 ER61

See also

Notes

assuming an inactive nucleus and a comet-like albedo of 0.05

Because 2015 ER61's orbit takes it so far from the Sun, a more accurate value for its orbit is a barycentric solution. Additionally, a close approach to Jupiter in 2016, and a travel through the inner solar system in 2017 drastically changes its orbit. Therefore, orbits for 2000–2016 and 2018–2100 are provided, respectively.

References

  1. ^ "C/2015 ER61 (PANSTARRS) Orbit". Minor Planet Center. Archived from the original on 2 March 2017. Retrieved 2 March 2017.
  2. ^ "JPL Small-Body Database Browser: (2015 ER61)" (last observation: 2016-01-23; arc: 1 yr). Jet Propulsion Laboratory. Archived from the original on 24 June 2015.
  3. ^ Gray, Bill. "Find_Orb Orbit Determination Software". Project PLuto. Retrieved 22 April 2019.
  4. "Glossary: Absolute Magnitude (H)". JPL. NASA. Archived from the original on 2 March 2001. Retrieved 14 September 2015.
  5. ^ "MPEC 2016-C01 : COMET C/2015 ER61 (PANSTARRS)". IAU Minor Planet Center. 1 February 2016. Retrieved 1 February 2016. (CK15E61R)
  6. Archive of JPL 13 (2015-Jun-04) as Amor near-Earth object
  7. Meech, Karen Jean; Sorli, Kya; Kleyna, Jan; Keane, Jacqueline; Bauer, James M.; Micheli, Marco; Schambeau, Charles Alfred; Sarid, Gal; Hainaut, Olivier; Yang, Bin; Wainscoat, Richard J.; Boe, Benjamin; Kramer, Emily A.; Bhatt, Bhuwan; Sahu, Devendra (2016). "Watching a Long Period Comet Turn On - C/2015 ER61 (PANSTARRS)". AAS/Division for Planetary Sciences Meeting Abstracts #48. 48: 308.06. Bibcode:2016DPS....4830806M.
  8. Seiichi Yoshida (27 February 2007). "C/2015 ER61 ( PanSTARRS )". Seiichi Yoshida's Comet Catalog. Retrieved 2 March 2017.

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