C/2006 E1 McNaught
more info
C/2006 E1 was discovered on 11 March 2006 by Robert H. McNaught on the Siding Spring Survey images taken with the 0.5-m Uppsala Schmidt telescope [IAUC 8688, 2006 March 16]. After perihelion passage in January 2007, it was ocassionally observed starting from 26 January 2008 until 3 March 2009 (see figure).
This comet made its closest approach to the Earth on 3 July 2006 (5.382 au), six months before perihelion.
Solution given here is based on data spanning over 3.0 yr in a range of heliocentric distances: 6.39 au – 6.041 au (perihelion) – 8.07 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system on hiperbolic orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
This comet made its closest approach to the Earth on 3 July 2006 (5.382 au), six months before perihelion.
Solution given here is based on data spanning over 3.0 yr in a range of heliocentric distances: 6.39 au – 6.041 au (perihelion) – 8.07 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to escape of the comet from the solar system on hiperbolic orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 143 | |
| data interval | 2006 03 11 – 2009 03 03 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.39 au – 6.04 au (perihelion) – 8.07 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 | 282 | |
| RMS [arcseconds] | 0.65 | |
| orbit quality class | 1a | |
| next 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 | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -46.61 – -43.68 – -40.86 | |
| next perihelion distance [au] | 254 – 261 – 269 | |
| synchronous stop epoch [Myr] | 1.95 | S |
| percentage of VCs with qnext > 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.
| next 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 | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -45.77 – -42.86 – -40.06 | |
| next perihelion distance [au] | 7.6 – 7.95 – 8.32 | |
| synchronous stop epoch [Myr] | 2.01 | S |
| percentage of VCs with qnext < 10 | 100 | |