C/2005 B1 Christensen
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C/2005 B1 was discovered by Eric Christensen on 16 January 2005 on Catalina Sky Survey images and its cometary apperance was soon confirmed [IAUC 8466, 2005 January 17]. Next, 2004 FS101 reported as asteroidal object by LINEAR and Spacewatch in March 2004 was identified with C/2005 B1 [IAUC 8469, 2005 January 19].
This comet made its closest approach to the Earth on 30 September 2006 (3.003 au), seven months after perihelion passage (see figure).
Solutions given here are based on data spanning over 3.6 yr in a range of heliocentric distances: 6.94 au – 3.205 au (perihelion) – 5.49 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
This comet made its closest approach to the Earth on 30 September 2006 (3.003 au), seven months after perihelion passage (see figure).
Solutions given here are based on data spanning over 3.6 yr in a range of heliocentric distances: 6.94 au – 3.205 au (perihelion) – 5.49 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 1517 | |
| data interval | 2004 03 18 – 2007 11 03 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.94 au – 3.21 au (perihelion) – 5.49 au | |
| detectability of NG effects in the comet's motion | comet with determinable NG~orbit | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 2991 | |
| RMS [arcseconds] | 0.45 | |
| orbit quality class | 1a+ | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 0 | |
| no. of escaping VCs in the swarm | 5001 | * |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 8.82 – 9.20 – 9.60 | |
| previous perihelion distance [au] | 3225 – 3258 – 3290 | |
| previous aphelion distance [103 au] | 205 – 214 – 223 | |
| time interval to previous perihelion [Myr] | 3.73 ± 13 | |
| 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 | 0 | |
| no. of escaping VCs in the swarm | 5001 | * |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 7.19 – 7.60 – 8.02 | |
| previous perihelion distance [au] | 4.46 – 4.62 – 4.79 | |
| previous aphelion distance [103 au] | 249 – 263 – 278 | |
| time interval to previous perihelion [Myr] | 3.73 ± 13 | |
| percentage of VCs with qprev < 10 | 100 | |