C/1947 Y1 Mrkos
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Comet C/1947 Y1 was discovered on 20 December 1947 by Antonín Mrkos (Skalnaté Pleso Observatory, Slovakia), that is two months before perihelion passage; the comet was last seen on 30 November 1948. [Kronk, Cometography: Volume 4].
This comet made its closest approach to the Earth on 17 February 1948 (1.674 au), that is almost at the moment of perihelion passage.
Solution given here is based on data spanning over 0.890 yr in a range of heliocentric distances from 1.589 au through perihelion (1.500 au) to 3.848 au.
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system, and it will enter the planet zone as Oort spike comet in the next perihelion passage (see future barycentric orbit).
More details in Królikowska et al. 2014.
This comet made its closest approach to the Earth on 17 February 1948 (1.674 au), that is almost at the moment of perihelion passage.
Solution given here is based on data spanning over 0.890 yr in a range of heliocentric distances from 1.589 au through perihelion (1.500 au) to 3.848 au.
This Oort spike comet suffers slight planetary perturbations during its passage through the planetary system, and it will enter the planet zone as Oort spike comet in the next perihelion passage (see future barycentric orbit).
More details in Królikowska et al. 2014.
| solution description | ||
|---|---|---|
| number of observations | 124 | |
| data interval | 1948 01 18 – 1948 11 30 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 1.59 au – 1.50 au (perihelion) – 3.85 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 | 204 | |
| RMS [arcseconds] | 1.22 | |
| orbit quality class | 1b | |
| 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] | 43.58 – 54.03 – 64.86 | |
| next perihelion distance [au] | 8.7 – 20 – 30 | |
| next aphelion distance [103 au] | 31 – 37 – 46 | |
| time interval to next perihelion [Myr] | 1.9 – 2.5 – 3.4 | |
| percentage of VCs with qnext < 10 | 13 | |
| percentage of VCs with 10 < qnext < 20 | 38 | |
| percentage of VCs with qnext > 20 | 49 | |
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] | 43.56 – 54.09 – 65.16 | |
| next perihelion distance [au] | 2.2 – 3 – 5.5 | |
| next aphelion distance [103 au] | 31 – 37 – 46 | |
| time interval to next perihelion [Myr] | 1.9 – 2.5 – 3.4 | |
| percentage of VCs with qnext < 10 | 98 | |
| percentage of VCs with 10 < qnext < 20 | 2 | |