C/2008 C1 Chen-Gao
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Comet C/2008 C1 was discovered on 1 February 2008 by Tao Chen (Suzhou City, Jiangsu province, China) and Xing Gao (Urumqi, Xinjiang province, China) at Xingming Observatory (Mt. Nanshan); that is about 2.5 months before its perihelion passage. A few pre-discovery images taken on 30 and 31 January at Xingming Observatory were next found. The comet was observed until 28 May 2008.
Comet had its closest approach to the Earth on 13 March 2008 (1.301 au), about 1.5 month after its discovery.
Solutions given here are based on data spanning over 0.323 yr in a range of heliocentric distances: 1.71 au – 1.262 au (perihelion) – 1.41 au. The non-gravitational solution was chosen as preferred orbit; however, uncertainties of NG parameters are large.
This comet suffers moderate planetary perturbations during its passage through the planetary system; these perturbations lead to more tight future orbit (see future barycentric orbits).
See also Królikowska and Dybczyński 2013 and Królikowska 2020.
Comet had its closest approach to the Earth on 13 March 2008 (1.301 au), about 1.5 month after its discovery.
Solutions given here are based on data spanning over 0.323 yr in a range of heliocentric distances: 1.71 au – 1.262 au (perihelion) – 1.41 au. The non-gravitational solution was chosen as preferred orbit; however, uncertainties of NG parameters are large.
This comet suffers moderate planetary perturbations during its passage through the planetary system; these perturbations lead to more tight future orbit (see future barycentric orbits).
See also Królikowska and Dybczyński 2013 and Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 802 | |
| data interval | 2008 01 30 – 2008 05 28 | |
| data type | almost all measurements before perihelion (PRE++) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 1.71 au – 1.26 au (perihelion) – 1.41 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 1544 | |
| RMS [arcseconds] | 0.36 | |
| orbit quality class | 2b | |
| next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 4989 | * |
| no. of escaping VCs in the swarm | 12 | |
| no. of hyperbolas among escaping VCs in the swarm | 6 | |
| next reciprocal semi-major axis [10-6 au-1] | 363.29 – 647.51 – 936.01 | R |
| next perihelion distance [au] | 1.263 – 1.265 – 1.267 | R |
| next aphelion distance [103 au] | 2.1 – 3.1 – 5.5 | R |
| time interval to next perihelion [Myr] | 0.035 – 0.06 – 0.14 | R |
| 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 | 4990 | * |
| no. of escaping VCs in the swarm | 11 | |
| no. of hyperbolas among escaping VCs in the swarm | 6 | |
| next reciprocal semi-major axis [10-6 au-1] | 363.28 – 647.51 – 936.01 | R |
| next perihelion distance [au] | 1.26259 – 1.2627 – 1.26274 | R |
| next aphelion distance [103 au] | 2.1 – 3.1 – 5.5 | R |
| time interval to next perihelion [Myr] | 0.035 – 0.06 – 0.14 | R |
| percentage of VCs with qnext < 10 | 100 | |