C/2002 A3 LINEAR
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C/2002 A3 was discovered on 13 January 2002 by the LINEAR as an apparently asteroidal object. Soon, its cometary apperance was reported [IAUC 7799, 2002 January 21].
This comet made its closest approach to the Earth on 12 January 2002 (4.395 au), 3.3 months before perihelion. Around perihelion the comet was not observed for almost 7.5 months (from 2 April to 10 November 2002).
Solution given here is based on data spanning over 1.4 yr in a range of heliocentric distances: 5.21 au – 5.151 au (perihelion) – 6.05 au.
C/2002 A3 had close encounter with Jupiter on 22 January 2003 (0.502 au). Planetary perturbationschanged the orbit of this comet significantly, and this originally Oort spike comet will leave the planetary zone in an orbit with semimajor axis of only about 160 au; thus, its orbital period has been shortened to about 2000 yr.
See also Królikowska 2014 and Wysoczańska et al., 2020.
This comet made its closest approach to the Earth on 12 January 2002 (4.395 au), 3.3 months before perihelion. Around perihelion the comet was not observed for almost 7.5 months (from 2 April to 10 November 2002).
Solution given here is based on data spanning over 1.4 yr in a range of heliocentric distances: 5.21 au – 5.151 au (perihelion) – 6.05 au.
C/2002 A3 had close encounter with Jupiter on 22 January 2003 (0.502 au). Planetary perturbationschanged the orbit of this comet significantly, and this originally Oort spike comet will leave the planetary zone in an orbit with semimajor axis of only about 160 au; thus, its orbital period has been shortened to about 2000 yr.
See also Królikowska 2014 and Wysoczańska et al., 2020.
| solution description | ||
|---|---|---|
| number of observations | 293 | |
| data interval | 2002 01 13 – 2003 06 24 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 5.21 au – 5.15 au (perihelion) – 6.05 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 | 579 | |
| RMS [arcseconds] | 0.49 | |
| orbit quality class | 1a | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 4445 | * |
| no. of escaping VCs in the swarm | 556 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 17.21 – 18.92 – 20.89 | R |
| previous perihelion distance [au] | 2490 – 2547 – 2560 | R |
| previous aphelion distance [103 au] | 93.2 – 103 – 114 | R |
| time interval to previous perihelion [Myr] | 10 – 12 – 14 | R |
| 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 | 4765 | * |
| no. of escaping VCs in the swarm | 236 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 17.99 – 19.99 – 22.20 | R |
| previous perihelion distance [au] | 69 – 120 – 220 | R |
| previous aphelion distance [103 au] | 90 – 99.9 – 111 | R |
| time interval to previous perihelion [Myr] | 9.6 – 11 – 13 | R |
| percentage of VCs with qprev > 20 | 100 | |