C/2007 D1 LINEAR
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C/2007 D1 was discovered on 17 February 2007 by the LINEAR as an apparently asteroidal object, however quickly its cometary appearance was reported.
This comet made its closest approaches to the Earth on 22 February (7.880 au, 4 months before perihelion passage, 5 days after its discovery) and 4 March 2008 (7.933 au, 8.5 months after perihelion).
Solution given here is based on data spanning over 6.2 yr in a range of heliocentric distances: 8.82 au – 8.794 au (perihelion) – 14.7 au.
This Oort spike comet suffers large planetary perturbations during its passage through the planetary system that lead to a notable more tight future orbit with the semimajor axis shorter than 2000 au (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
This comet made its closest approaches to the Earth on 22 February (7.880 au, 4 months before perihelion passage, 5 days after its discovery) and 4 March 2008 (7.933 au, 8.5 months after perihelion).
Solution given here is based on data spanning over 6.2 yr in a range of heliocentric distances: 8.82 au – 8.794 au (perihelion) – 14.7 au.
This Oort spike comet suffers large planetary perturbations during its passage through the planetary system that lead to a notable more tight future orbit with the semimajor axis shorter than 2000 au (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 548 | |
| data interval | 2007 02 17 – 2013 05 04 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 8.82 au – 8.79 au (perihelion) – 14.7 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 | 1061 | |
| RMS [arcseconds] | 0.45 | |
| orbit quality class | 1a+ | |
| 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] | 737.15 – 738.36 – 739.58 | |
| next perihelion distance [au] | 8.79096 – 8.79098 – 8.79101 | |
| next aphelion distance [103 au] | 2.695 – 2.7 – 2.704 | |
| time interval to next perihelion [Myr] | 0.0494 – 0.04952 – 0.04964 | |
| percentage of VCs with qnext < 10 | 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.
| 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] | 737.14 – 738.36 – 739.58 | |
| next perihelion distance [au] | 8.7879 – 8.78791 – 8.78793 | |
| next aphelion distance [103 au] | 2.695 – 2.7 – 2.704 | |
| time interval to next perihelion [Myr] | 0.04936 – 0.04949 – 0.04961 | |
| percentage of VCs with qnext < 10 | 100 | |