C/2003 T3 Tabur
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Comet C/2003 T3 was discovered on 14 October 2003 by Vello Tabur (Australian Capital Territory); that is 6.5 months before its perihelion passage. It was observed until 3 May 2005.
Comet had its closest approach to the Earth on 22 May 2004 (2.319 au), about 3 weeks after its perihelion passage.
Preferred solution given here is based on data spanning over 1.55 yr in a range of heliocentric distances: 2.968 au – 1.481 au (perihelion) – 4.63 au, however NG solution based on pre-perihelion data (pn) is also adequate for past calculations.
This Oort spike comet suffers large planetary perturbations during its passage through the planetary system; these perturbations lead to a significantly more tight future orbit with semimajor axis of about 1,400 au.
See also Królikowska 2020.
Comet had its closest approach to the Earth on 22 May 2004 (2.319 au), about 3 weeks after its perihelion passage.
Preferred solution given here is based on data spanning over 1.55 yr in a range of heliocentric distances: 2.968 au – 1.481 au (perihelion) – 4.63 au, however NG solution based on pre-perihelion data (pn) is also adequate for past calculations.
This Oort spike comet suffers large planetary perturbations during its passage through the planetary system; these perturbations lead to a significantly more tight future orbit with semimajor axis of about 1,400 au.
See also Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 769 | |
| data interval | 2003 10 14 – 2005 05 03 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 2.96 au – 1.48 au (perihelion) – 4.63 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 | 1522 | |
| RMS [arcseconds] | 0.61 | |
| 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] | 736.95 – 737.85 – 738.76 | |
| next perihelion distance [au] | 1.47524 – 1.47524 – 1.47525 | |
| next aphelion distance [103 au] | 2.706 – 2.709 – 2.712 | |
| time interval to next perihelion [Myr] | 0.04947 – 0.04956 – 0.04965 | |
| 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] | 736.95 – 737.85 – 738.76 | |
| next perihelion distance [au] | 1.47673 – 1.47674 – 1.47674 | |
| next aphelion distance [103 au] | 2.706 – 2.709 – 2.712 | |
| time interval to next perihelion [Myr] | 0.04945 – 0.04955 – 0.04964 | |
| percentage of VCs with qnext < 10 | 100 | |