C/2005 L3 McNaught
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C/2005 L3 was discovered by R.H. McNaught with the 0.5-m Uppsala Schmidt in the course of the Siding Spring Survey on 3 June 2005 [IAUC 8536, 2005 June 7]. Later, prediscovery detections by Siding Spring Survey were found (16 July and 16 August 2004, see figure).
This comet made two closest approaches to the Earth on 24 June 2007 (4.852 au, almost seven months before perihelion) and 12 May 2008 (4.857 au, four months after perihelion).
Solutions given here are based on data spanning over 9.48 yr (10 oppositions) in a range of heliocentric distances: 10.3 au – 5.593 au (perihelion) – 14.9 au.
NG orbit using full data-arc is determinable.
This Oort spike comet suffers rather 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 and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
This comet made two closest approaches to the Earth on 24 June 2007 (4.852 au, almost seven months before perihelion) and 12 May 2008 (4.857 au, four months after perihelion).
Solutions given here are based on data spanning over 9.48 yr (10 oppositions) in a range of heliocentric distances: 10.3 au – 5.593 au (perihelion) – 14.9 au.
NG orbit using full data-arc is determinable.
This Oort spike comet suffers rather 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 and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
| solution description | ||
|---|---|---|
| number of observations | 5339 | |
| data interval | 2004 07 16 – 2014 01 09 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 10.3 au – 5.59 au (perihelion) – 14.93 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 | 10453 | |
| RMS [arcseconds] | 0.50 | |
| orbit quality class | 1a+ | |
| 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] | 61.49 – 61.65 – 61.82 | |
| previous perihelion distance [au] | 8.303 – 8.326 – 8.349 | |
| previous aphelion distance [103 au] | 32.34 – 32.43 – 32.52 | |
| time interval to previous perihelion [Myr] | 2.054 – 2.062 – 2.071 | |
| percentage of VCs with qprev < 10 | 100 | |
Upper panel: 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.
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
| 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] | 61.49 – 61.66 – 61.82 | |
| previous perihelion distance [au] | 7.838 – 7.861 – 7.884 | |
| previous aphelion distance [103 au] | 32.34 – 32.43 – 32.52 | |
| time interval to previous perihelion [Myr] | 2.054 – 2.062 – 2.07 | |
| percentage of VCs with qprev < 10 | 100 | |