C/2014 OE4 PANSTARRS
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Comet C/2014 OE4 was discovered on 26 July 2014 with Pan-STARRS 1 telescope (Haleakala), that is 2.4 yr before its perihelion passage; its cometary nature was soon recognised. Next, this comet was found on earlier images taken on several occasion by Pan-STARRS 1, Mount Lemmon Survey and Steward Observatory (Kitt Peak-Spacewatch survey), reaching back to 8 May 2014. This comet was observed until the end of 2019, and is still observable.
Comet had its closest approach to the Earth on 1 June 2016 (5.755 au), about six months before its perihelion passage.
Solution given here is based on data spanning over 3.78 yr in a range of heliocentric distances: 8.86 au – 6.253 au (perihelion) – 6.91 au (18 February 2018).
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit with a semimajor axis larger than 10,000 au (see future barycentric orbits).
Comet had its closest approach to the Earth on 1 June 2016 (5.755 au), about six months before its perihelion passage.
Solution given here is based on data spanning over 3.78 yr in a range of heliocentric distances: 8.86 au – 6.253 au (perihelion) – 6.91 au (18 February 2018).
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit with a semimajor axis larger than 10,000 au (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 1373 | |
| data interval | 2014 05 08 – 2018 02 18 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 8.86 au – 6.24 au (perihelion) – 6.91 au | |
| detectability of NG effects in the comet's motion | NG effects not determinable | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 2691 | |
| RMS [arcseconds] | 0.31 | |
| orbit quality class | 1a+ | |
| next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| next reciprocal semi-major axis [10-6 au-1] | 97.19 – 97.55 – 97.92 | |
| next perihelion distance [au] | 6.27879 – 6.27892 – 6.27901 | |
| next aphelion distance [103 au] | 20.42 – 20.5 – 20.57 | |
| time interval to next perihelion [Myr] | 1.03 – 1.036 – 1.042 | |
| percentage of VCs with qnext < 10 | 100 | |
| next orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| next reciprocal semi-major axis [10-6 au-1] | 97.19 – 97.55 – 97.92 | |
| next perihelion distance [au] | 6.27771 – 6.27813 – 6.27854 | |
| next aphelion distance [103 au] | 20.42 – 20.5 – 20.57 | |
| time interval to next perihelion [Myr] | 1.031 – 1.036 – 1.042 | |
| percentage of VCs with qnext < 10 | 100 | |