C/2004 X3 LINEAR
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C/2004 X3 was discovered on 15 December 2004 by the LINEAR as an apparently asteroidal object. In the following week its cometary apperance was reported by observers [IAUC 8457, 2004 December 21]. At the moment of discovery, it was 6 months before its perihelion passage (see figure).
This comet made its closest approach to the Earth on 9 March 2005 (3.499 au), 3.3 months before perihelion.
Solution given here is based on data spanning over 1.3 yr in a range of heliocentric distances: 4.65 au – 4.402 au (perihelion) – 4.98 au.
This Oort spike comet suffers notable planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system on hiperbolic orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
This comet made its closest approach to the Earth on 9 March 2005 (3.499 au), 3.3 months before perihelion.
Solution given here is based on data spanning over 1.3 yr in a range of heliocentric distances: 4.65 au – 4.402 au (perihelion) – 4.98 au.
This Oort spike comet suffers notable planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system on hiperbolic orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 250 | |
| data interval | 2004 12 15 – 2006 03 31 | |
| data type | significantly more measurements before perihelion (PRE+) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 4.65 au – 4.40 au (perihelion) – 4.98 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 | 487 | |
| RMS [arcseconds] | 0.51 | |
| orbit quality class | 1a | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 1930 | |
| no. of escaping VCs in the swarm | 3071 | * |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 13.14 – 15.60 – 17.93 | |
| previous perihelion distance [au] | 2400 – 2900 – 3500 | R |
| previous aphelion distance [103 au] | 110 – 130 – 150 | |
| time interval to previous perihelion [Myr] | 11.6 – 13.2 – 14.2 | 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 | 660 | |
| no. of escaping VCs in the swarm | 4341 | * |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 11.45 – 14.14 – 16.69 | |
| previous perihelion distance [au] | 10 – 12 – 15 | |
| previous aphelion distance [103 au] | 120 – 140 – 170 | |
| time interval to previous perihelion [Myr] | 3.56 ± 3.3 | |
| percentage of VCs with qprev < 10 | 9 | |
| percentage of VCs with 10 < qprev < 20 | 91 | |