C/2013 V4 Catalina
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Comet C/2013 V4 was discovered on 9 November 2013 with Catalina Sky Survey, that is less than one year before its perihelion passage. Next, it was found on earlier images taken on 23 October 2013 with the Pan-STARRS 1, Haleakala, and 31 October 2013 with Catalina Sky Survey. This comet was observed until 6 August 2018.
Comet had its closest approach to the Earth on 1 December 2015 (4.535 au), less than 2 months after its perihelion passage.
Solution given here is based on data spanning over 4.79 yr in a range of heliocentric distances: 7.35 au – 5.185 au (perihelion) – 8.99 au.
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit (see future barycentric orbits).
Comet had its closest approach to the Earth on 1 December 2015 (4.535 au), less than 2 months after its perihelion passage.
Solution given here is based on data spanning over 4.79 yr in a range of heliocentric distances: 7.35 au – 5.185 au (perihelion) – 8.99 au.
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 2454 | |
| data interval | 2013 10 23 – 2018 08 06 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 7.35 au – 5.18 au (perihelion) – 8.99 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 | 4865 | |
| RMS [arcseconds] | 0.48 | |
| orbit quality class | 1a+ | |
| next orbit elements (barycentric ecliptic J2000) | ||
|---|---|---|
| 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 recip semi-major axis [10-6 au-1] | 156.95 ± 0.24 | |
| next perihelion distance [au] | 5.2123 ± 0.0004 | |
| next aphelion distance [103 au] | 12.74 ± 0.02 | |
| time interval to next perihelion [Myr] | 0.508 ± 0.001 | |
| percentage of VCs with q < 10 | 100 | |
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.