C/2006 P1 McNaught
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Comet C/2006 P1 was discovered on 7 August 2006 by Robert H. McNaught (Siding Spring Survey); that is about 5 months before its perihelion passage. It was observed until 11 July 2007 (see picture).
This comet with small perihelion distance of 0.17 au was the second brightest comet observed by ground-based observers since 1935 and developed a spectacularly structured huge dust tail.
Comet had its closest approach to the Earth on 15 January 2007 (0.817 au), about 3 days after its perihelion passage.
All orbits presented here are based on data spanning over 0.926 yr in a range of heliocentric distances: 2.74 au – 0.170 au (perihelion) – 3.34 au. NG orbit obtained using standard form of g(r) functionwith radial and transverse components of NG acceleration is quite well determined and was chosen here as preferred orbit; however, the NG orbit with three components of NG accelarations is also worth the attention.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system and these perturbations lead to more tight future orbit with semimajor axis a bit larger than 2,000 au (see future barycentric orbits).
See also Królikowska and Dybczyński 2013 and Królikowska 2020.
This comet with small perihelion distance of 0.17 au was the second brightest comet observed by ground-based observers since 1935 and developed a spectacularly structured huge dust tail.
Comet had its closest approach to the Earth on 15 January 2007 (0.817 au), about 3 days after its perihelion passage.
All orbits presented here are based on data spanning over 0.926 yr in a range of heliocentric distances: 2.74 au – 0.170 au (perihelion) – 3.34 au. NG orbit obtained using standard form of g(r) functionwith radial and transverse components of NG acceleration is quite well determined and was chosen here as preferred orbit; however, the NG orbit with three components of NG accelarations is also worth the attention.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system and these perturbations lead to more tight future orbit with semimajor axis a bit larger than 2,000 au (see future barycentric orbits).
See also Królikowska and Dybczyński 2013 and Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 334 | |
| data interval | 2006 08 07 – 2007 07 11 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 2.74 au – 0.17 au (perihelion) – 3.34 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 641 | |
| RMS [arcseconds] | 0.25 | |
| orbit quality class | 1b | |
| previous 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 | |
| previous reciprocal semi-major axis [10-6 au-1] | 48.95 – 57.20 – 62.34 | |
| previous perihelion distance [au] | 0.14 – 0.4 – 84 | |
| previous aphelion distance [103 au] | 32.1 – 35 – 40.8 | |
| time interval to previous perihelion [Myr] | 2 – 2.3 – 2.7 | |
| percentage of VCs with qprev < 10 | 77 | |
| percentage of VCs with 10 < qprev < 20 | 3 | |
| percentage of VCs with qprev > 20 | 20 | |
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 | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 51.97 – 57.27 – 62.33 | |
| previous perihelion distance [au] | 0.055 – 0.079 – 0.098 | |
| previous aphelion distance [103 au] | 32.1 – 34.9 – 38.5 | |
| time interval to previous perihelion [Myr] | 2 – 2.3 – 2.7 | |
| percentage of VCs with qprev < 10 | 100 | |