C/2004 P1 NEAT
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C/2004 P1 was discovered on 5 August 2004 by the LINEAR as a faint diffuse comet. In the following days, its cometary apperance was confirmed [IAUC 8383, 2004 August 8]. Later, three pre-discovery detections by AMOS were found (11 May 2003, and 8, 21 July 2003). At the moment of discovery, it was one year after its perihelion passage (see figure).
This comet made its closest approach to the Earth on 20 July 2003 (5.233 au), 19 days before perihelion.
Solution given here is based on data spanning over 2.3 yr in a range of heliocentric distances: 6.05 au – 6.014 au (perihelion) – 7.91 au.
This Oort spike comet suffers small 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 20 July 2003 (5.233 au), 19 days before perihelion.
Solution given here is based on data spanning over 2.3 yr in a range of heliocentric distances: 6.05 au – 6.014 au (perihelion) – 7.91 au.
This Oort spike comet suffers small 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 | 151 | |
| data interval | 2003 05 11 – 2005 08 30 | |
| data type | significantly more measurements after perihelion (POST+) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.05 au – 6.01 au (perihelion) – 7.91 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 | 298 | |
| RMS [arcseconds] | 0.63 | |
| orbit quality class | 1a | |
| previous 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 | |
| previous reciprocal semi-major axis [10-6 au-1] | 26.69 – 30.66 – 34.63 | |
| previous perihelion distance [au] | 759 – 838 – 853 | |
| previous aphelion distance [103 au] | 57 – 64 – 74 | |
| time interval to previous perihelion [Myr] | 4.7 – 5.8 – 7.1 | |
| 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 | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 27.28 – 31.21 – 35.09 | |
| previous perihelion distance [au] | 20 – 31 – 57 | |
| previous aphelion distance [103 au] | 57 – 64 – 73 | |
| time interval to previous perihelion [Myr] | 4.8 – 5.7 – 7 | |
| percentage of VCs with 10 < qprev < 20 | 11 | |
| percentage of VCs with qprev > 20 | 89 | |