C/2005 Q1 LINEAR
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C/2005 Q1 was discovered on 27 August 2005 by the LINEAR as an apparently asteroidal object. At once its cometary apperance was reported by several observers [IAUC 8590, 2005 August 29]. At the moment of discovery, it was two days after perihelion passage.
This comet made its closest approaches to the Earth on 16 December 2004 (5.739 au, 8 months before perihelion passage) and 23 November 2005 (5.856 au, 3 months after perihelion).
Solution given here is based on data spanning over 2.1 yr in a range of heliocentric distances from 6.41 au to 8.25 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 approaches to the Earth on 16 December 2004 (5.739 au, 8 months before perihelion passage) and 23 November 2005 (5.856 au, 3 months after perihelion).
Solution given here is based on data spanning over 2.1 yr in a range of heliocentric distances from 6.41 au to 8.25 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 | 161 | |
| data interval | 2005 08 27 – 2007 10 16 | |
| data type | observed only after perihelion (POST) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.41 au – 8.25au | |
| 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 | 309 | |
| RMS [arcseconds] | 0.48 | |
| 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] | 20.01 – 22.54 – 24.96 | |
| previous perihelion distance [au] | 2390 – 2670 – 2910 | |
| previous aphelion distance [103 au] | 77.7 – 86.1 – 97.1 | |
| time interval to previous perihelion [Myr] | 7.7 – 9 – 11 | |
| 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] | 20.00 – 22.74 – 25.36 | |
| previous perihelion distance [au] | 42 – 69 – 130 | |
| previous aphelion distance [103 au] | 79 – 88 – 100 | |
| time interval to previous perihelion [Myr] | 7.8 – 9.2 – 11 | |
| percentage of VCs with qprev > 20 | 100 | |