C/2017 K5 PANSTARRS
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Comet C/2017 K5 was discovered on 27 May 2017 with Pan-STARRS 1 telescope (Haleakala), that is almost 3 years before its perihelion passage. This comet was observed until 9 July 2020.
Comet will have its closest approach to the Earth on 2 July 2020 (6.688 au), a bit more than a 3 months after its perihelion passage.
The preferred solution given here is based on pre-perihelion data spanning over 3.12 yr in a range of heliocentric distances from 9.90 au – 7.68 au (perihelion) – 7.71 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that likely lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits).
Comet will have its closest approach to the Earth on 2 July 2020 (6.688 au), a bit more than a 3 months after its perihelion passage.
The preferred solution given here is based on pre-perihelion data spanning over 3.12 yr in a range of heliocentric distances from 9.90 au – 7.68 au (perihelion) – 7.71 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that likely lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 25 | |
| data interval | 2017 05 27 – 2018 05 12 | |
| data arc selection | data generally limited to pre-perihelion (PRE) | |
| range of heliocentric distances | 9.9 au – 8.74au | |
| detectability of NG effects in the comet's motion | NG effects not determinable | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | NO | |
| number of residuals | 50 | |
| RMS [arcseconds] | 0.35 | |
| orbit quality class | 1b | |
| previous 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 | |
| previous reciprocal semi-major axis [10-6 au-1] | 47.19 – 66.88 – 79.61 | |
| previous perihelion distance [au] | 7.461 – 7.499 – 7.635 | |
| previous aphelion distance [103 au] | 25 – 30 – 42 | |
| time interval to previous perihelion [Myr] | 1.4 – 1.8 – 2.5 | |
| percentage of VCs with qprev < 10 | 90 | |
| percentage of VCs with 10 < qprev < 20 | 1 | |
| percentage of VCs with qprev > 20 | 9 | |
Time distribution of positional observations with corresponding heliocentric (red curve) and geocentric (green curve) distance at which they were taken. The horizontal dotted line shows the perihelion distance for a given comet whereas vertical dotted line — the moment of perihelion passage.
| previous 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 | |
| previous reciprocal semi-major axis [10-6 au-1] | 53.98 – 66.90 – 79.59 | |
| previous perihelion distance [au] | 7.6669 – 7.6745 – 7.7208 | |
| previous aphelion distance [103 au] | 25 – 30 – 37 | |
| time interval to previous perihelion [Myr] | 1.4 – 1.8 – 2.5 | |
| percentage of VCs with qprev < 10 | 100 | |