C/1950 K1 Minkowski
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Comet C/1950 K1 was discovered on 19 May 1950 by Rudolf L.B. Minkowski (Palomar Observatory, California, USA). At the moment of discovery, the comet was almost 9 months before perihelion passage and it was last seen on 19 January 1953. [Kronk, Cometography: Volume 4].
This comet made its closest approach to the Earth on 23 March 1951 (1.774 au), that is over two months after perihelion passage.
Solution given here is based on data spanning over 2.652 yr in a range of heliocentric distances from 3.531 au through perihelion (2.572 au) to 7.258 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that cause a bit tighter future orbit (see original and future barycentric orbits).
More details in Królikowska et al. 2014.
This comet made its closest approach to the Earth on 23 March 1951 (1.774 au), that is over two months after perihelion passage.
Solution given here is based on data spanning over 2.652 yr in a range of heliocentric distances from 3.531 au through perihelion (2.572 au) to 7.258 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that cause a bit tighter future orbit (see original and future barycentric orbits).
More details in Królikowska et al. 2014.
| solution description | ||
|---|---|---|
| number of observations | 254 | |
| data interval | 1950 05 27 – 1953 01 19 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 3.53 au – 2.57 au (perihelion) – 7.26 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 | 466 | |
| RMS [arcseconds] | 1.28 | |
| 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] | 275.52 – 278.35 – 281.17 | |
| next perihelion distance [au] | 2.57891 – 2.57892 – 2.57894 | |
| next aphelion distance [103 au] | 7.11 – 7.18 – 7.26 | |
| time interval to next perihelion [Myr] | 0.212 – 0.215 – 0.218 | |
| percentage of VCs with qnext < 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.
| 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] | 275.53 – 278.36 – 281.18 | |
| next perihelion distance [au] | 2.57206 – 2.57211 – 2.57217 | |
| next aphelion distance [103 au] | 7.11 – 7.18 – 7.26 | |
| time interval to next perihelion [Myr] | 0.212 – 0.215 – 0.218 | |
| percentage of VCs with qnext < 10 | 100 | |