C/1987 W3 Jensen-Shoemaker
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Comet C/1987 W3 was discovered by Carolyn S. and Eugene M. Shoemaker (with the 0.46-m Schmidt telescope at Palomar) on 24 November 1987 (IAUC 4503), when the comet was about two months before its perihelion passage. It was next announced (IAUC 4505) that the same comet was discovered by Poul Jensen on an earlier exposure taken by Karl Augustesen on 25 October (with the 0.45-m Schmidt telescope at the Copenhagen Observatory's Brorfelde station). Later, two more pre-discovery observations from September were found. The comet was last seen on 29 April 1990.
C/1987 W3 made its closest approach to the Earth on 17 October 1987 (2.47 au), that was three months before its perihelion passage.
Solution given here is based on data spanning over 2.60 yr in a range of heliocentric distances: 3.51 au – 3.33 au (perihelion) – 7.77 au.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
C/1987 W3 made its closest approach to the Earth on 17 October 1987 (2.47 au), that was three months before its perihelion passage.
Solution given here is based on data spanning over 2.60 yr in a range of heliocentric distances: 3.51 au – 3.33 au (perihelion) – 7.77 au.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 34 | |
| data interval | 1987 09 24 – 1990 04 29 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 3.51 au – 3.33 au (perihelion) – 7.77 au | |
| 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 | 65 | |
| RMS [arcseconds] | 1.22 | |
| orbit quality class | 1a | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 3889 | * |
| no. of escaping VCs in the swarm | 1112 | |
| no. of hyperbolas among escaping VCs in the swarm | 17 | |
| previous reciprocal semi-major axis [10-6 au-1] | 11.60 – 22.58 – 33.70 | |
| previous perihelion distance [au] | 76 – 120 – 420 | R |
| previous aphelion distance [103 au] | 59 – 88 – 170 | |
| time interval to previous perihelion [Myr] | 5.2 – 8.1 – 12 | R |
| percentage of VCs with qprev > 20 | 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.
| previous orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 4539 | * |
| no. of escaping VCs in the swarm | 462 | |
| no. of hyperbolas among escaping VCs in the swarm | 1 | |
| previous reciprocal semi-major axis [10-6 au-1] | 18.06 – 25.63 – 34.18 | R |
| previous perihelion distance [au] | 15 – 65 – 470 | R |
| previous aphelion distance [103 au] | 59 – 78 – 110 | R |
| time interval to previous perihelion [Myr] | 4.9 – 7.3 – 11 | R |
| percentage of VCs with qprev < 10 | 4 | |
| percentage of VCs with 10 < qprev < 20 | 13 | |
| percentage of VCs with qprev > 20 | 83 | |